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Astronomy & Astrophysics manuscript no. 26199 July 23, 2015

c ESO 2015

Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919
´ R. Cesaroni1 , F. Massi1 , C. Arcidiacono1,2 , M.T. Beltran1 , P. Persi3 , M. Tapia4 , S. Molinari3 , L. Testi5,1 , L. Busoni1 , 1 , K. Boutsia6 , S. Bisogni7,1 , D. McCarthy8 , and C. Kulesa8 A. Riccardi
1 2 3 4 5 6 7 8

INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy cesa,fmassi,mbeltran,riccardi,lbusoni@arcetri.astro.it INAF, Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy carmelo.arcidiacono@oabo.inaf.it INAF, Istituto di Astrofisica e Planetologia Spaziale, Via Fosso del Cavaliere 100, I-00133, Roma, Italy paolo.persi,sergio.molinari@iaps.inaf.it ´ ´ Instituto de Astronom´ , Universidad Nacional Autonoma de Mexico, Apdo. Postal 877, Ensenada, B. C., CP 22830, Mexico ia mt@astrosen.unam.mx European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748, Garching, Germany e-mail: ltesti@eso.org INAF, Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monte Porzio Catone, Italy konstantina.boutsia@oa-roma.inaf.it ` Universita degli Studi di Firenze, Via Sansone 1, I-50019 Sesto Fiorentino, Italy e-mail: susanna@arcetri.inaf.it Steward Observatory, The University of Arizona, 933 N. Cherry Ave., Tucson, AZ-85721, U.S.A. dwmccarthy@gmail.com, ckulesa@as.arizona.edu

e-mail: e-mail: e-mail: e-mail: e-mail: e-mail:

Received date; accepted date
ABSTRACT

Context. We present a study of the complex high-mass star forming region IRAS 05137+3919 (also known as Mol8), where multiple jets and a rich stellar cluster have been described in previous works. Aims. Our goal is to determine the number of jets and shed light on their origin, and thus determine the nature of the young stars powering these jets. We also wish to analyse the stellar clusters by resolving the brightest group of stars. Methods. The star forming region was observed in various tracers and the results were complemented with ancillary archival data. The new data represent a substantial improvement over previous studies both in resolution and frequency coverage. In particular, adaptive optics provides us with an angular resolution of 80 mas in the near IR, while new mid- and far-IR data allow us to sample the peak of the spectral energy distribution and thus reliably estimate the bolometric luminosity. Results. Thanks to the near-IR continuum and millimetre line data we can determine the structure and velocity field of the bipolar jets and outflows in this star forming region. We also find that the stars are grouped into three clusters and the jets originate in the richest of these, whose luminosity is 2.4 â 104 L . Interestingly, our high-resolution near-IR images allow us to resolve one of the two brightest stars (A and B) of the cluster into a double source (A1+A2). Conclusions. We confirm that there are two jets and establish that they are powered by B-type stars belonging to cluster C1. On this basis and on morphological and kinematical arguments, we conclude that the less extended jet is almost perpendicular to the line of sight and that it originates in the brightest star of the cluster, while the more extended one appears to be associated with the more extincted, double source A1+A2. We propose that this is not a binary system, but a small bipolar reflection nebula at the root of the large-scale jet, outlining a still undetected circumstellar disk. The gas kinematics on a scale of 0.2 pc seems to support our hypothesis, because it appears to trace rotation about the axis of the associated jet.
Key words. Stars: early-type ­ Stars: formation ­ ISM: jets and outflows

1. Introduction
Observationally, the study of high-mass star formation is severely hindered by the difficulty of identifying the object of interest in a crowded region. This is basically the result of the large distances of OB-type stars (typically, several kpc) and the presence of numerous, lower mass stars in the same field. As a matter of fact, OB-type stars form in rich clusters, which makes it difficult to distinguish the phenomena associated with the highmass star(s) of interest from those associated with other cluster members. High angular resolution is thus crucial for this type of investigation, since the (projected) separation inside these rich stellar cluster may be 1 . Resolutions that high can be attained by IR and radio interferometers as well as by 8-m class

Send offprint requests to: R. Cesaroni, e-mail: cesa@arcetri.astro.it Based on observations carried out with the Large Binocular Telescope. The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are: The University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; The Ohio State University, and The Research Corporation, on behalf of The University of Notre Dame, University of Minnesota, and University of Virginia.


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

telescopes operating at IR wavelengths, which are made possible through adaptive optics techniques. With this in mind, we have focused our attention on a massive star forming region, where evidence of multiple, young stellar objects (YSOs) was found. The corresponding counterpart in the IRAS PSC is IRAS 05137+3919, also known as Mol 8 from the catalogue of Molinari et al. (1996). These authors quote a kinematic distance of 10.8 kpc and a corresponding luminosity (estimated from the IRAS fluxes) of 5.6 â 104 L . Recently, Honma et al. (2011) have measured the parallax of the water +5 3 masers in this object, resulting in a distance of 11.6-2..8 kpc. The same authors also establish a lower limit of 8.3 kpc. This is consistent with a more recent parallax measurement by Reid +3 4 et al. (2014), who derive a distance of 7.7-1..8 kpc, implying an uncertainty of a factor 2 in luminosity. In the following, we adopt the minimum distance of 8.3 kpc estimated by Honma et al. (2011), with the caveat that higher values are possible. IRAS 05137+3919 does not satisfy the colour constraints established by Wood & Churchwell (1989) to identify (UC) HII regions in the IRAS PSC, because the colour index [60­12]=1.29 lies ­ although marginally ­ below the limit of 1.3. Indeed, despite the luminosity above 104 L , the source was not detected at 6 cm and 2 cm by Molinari et al. (1998), while only weak, compact continuum emission (0.33 mJy; Molinari et al. 2002) was measured at 3.6 cm. Whether this originates in an HII region or in a thermal jet still needs to be understood, but it appears likely that the 3.6 cm continuum emission is associated with one of the members of the embedded stellar cluster detected in the near IR by various authors (Ishii et al. 1998, 2002; Varricat et al. 2010) and studied by Faustini et al. (2009), Kumar et al. (2006), and Nikoghosyan & Azatyan (2014, 2015). The most likely candidates for ionising the radio source are two bright stars located at the centre of the cluster and already identified by Varricat et al. (2010). Interstingly, that cluster lies also close to the geometrical center of a bipolar outflow mapped in the 12 CO(1­0) line by Zhang et al. (2001, 2005). Varricat et al. (2010) imaged two bipolar jets in the H2 v=1­0 S(1) line, also centred on the stellar cluster and directed approximately NE­SW and NW­SE. Hereafter, we refer to these, respectively, as Jet 1 and Jet 2, following Varricat et al. (2010). The former is roughly oriented like the 12 CO outflow by Zhang et al. (2001, 2005) and the HCO+ (1­0) outflow mapped by Molinari et al. (2002) with the OVRO interferometer. The presence of shocked H2 emission is confirmed by the near-IR spectra obtained by Ishii et al. (2001), which refer to the NW­SE jet. Based on these previous findings, we decided to perform a multi-wavelength study of IRAS 05137+3919 with the main goal to relate the properties of the stellar cluster to those of the outflows/jets and hence identify the sources powering the flows and establish their nature. For these purposes, we obtained outflow maps a factor 4 better in angular resolution than those by Zhang et al. (2005) and imaged the stellar cluster with an 8-m class telescope employing adaptive optics to attain 0. 08. We also used the continuum far-IR images of the Herschel/Hi-GAL survey (Molinari et al. 2010) to accurately estimate the cluster luminosity. After describing the observational details in Sect. 2, we illustrate the results in Sect. 3, while the analysis and discussion of our findings is presented in Sect. 4. Finally, the conclusions are drawn in Sect. 5.

2. Observations and data reduction
2.1. Large Binocular Telescope
2.1.1. Near-IR images with LUCI

Near-IR images were taken in the night of December 12, 2009 with LUCI (Seifert et al. 2003) at the Large Binocular Telescope (Mount Graham, Arizona), through the standard broad-band filters H (c = 1.653 µm) and Ks (c = 2.163 µm), and the narrowband filters F eI I (c = 1.646 µm, including the [FeII] 1.64-µm line) and H2 (c = 2.122 µm, including the H2 v=1­0 S (1) line at 2.12 µm). We used the N3.75 camera with a pixel scale of 0. 12 and a field of view of 4 â4 . We took ten dithered images both at H and at Ks , each composed of 17 coadds of 2 s exposures (H ) and 15 coadds of 2 s exposures (Ks ). A set of 14 dithered images, each resulting from coadding five exposures of 20 s, were taken at H2 , whereas eight dithered images were taken at F eI I , each of them a coadd of nine exposures of 20 s. Total exposure times were then 300 s (Ks ), 340 s (H ), 1400 s (H2 ), and 1440 s (F eI I ), respectively. The dithering pattern consisted in alternatively imaging the target in the central part, the eastern part, and the western part of the detector field (i.e., with a throw of 1 in right ascension), with a random jitter of a few arcsec when the target was in the same area of the detector. These allowed us to obtain sky images from the on-source images themselves, by median filtering together 4 frames selected so that the target area did not overlap in the stack, which would have been a problem due to the extended emission feature in the field centre. All the images were flat-fielded, bad-pixel corrected, skysubtracted, registered, and combined by using standard IRAF1 routines. We note that, given the dithering strategy adopted, all final combined images attain their maximum signal-to-noise ratio in a central area 2 wide in right ascension. The full width at half maximum (FWHM) of the point-spread function (PSF) was between 0. 5 and 0. 6. We scaled the Ks and H2 final mosaics appropriately (by assuming a constant stellar continuum flux, which is correct only as a zero-order approximation) and then subtracted one from the other, to obtain a continuum-free map of pure H2 line emission. In practice, we solved the two equations that give the intensities measured in the H2 and Ks filters I
H2

= =

S S

H2 H2

c d + S c d + S

H2

t

H2



H2

(1) (2)

I

K

s

K

s

t Ks

K

s

H H c c with respect to S 2 d and S , where S 2 and S are the H2 line and continuum flux densities, H2 and Ks the widths of the H2 and Ks filters, tH2 and tKs the corresponding integration times, and H2 and Ks the transparencies of the two filters. We followed the same procedure with the H and F eI I final mosaics, but no [FeII] emission could be detected in the subtracted image, so we do not discuss the [FeII] data further. We performed PSF-fit photometry on the Ks and H final averaged (mosaiced) images by using the DAOPHOT routines in IRAF. In total, we found 1303 sources with detection at both Ks and H , 143 sources with detection at Ks and 60 sources with detection at H (see Table A.1). Unfortunately, the standard

IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Associated Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.

1


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

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Fig. 1. Maps of the continuum emission towards IRAS 05137+3919 at different wavelengths (given in the top right of each panel). The labels in the top, right panel indicate the three clumps/clusters that we refer to in the text. The images have been taken from our LUCI data (2.2 µm), the IRAC database (at 3.4 and 4.6 µm), the WISE archive (12 and 22 µm), the Herschel/Hi-GAL survey (70­250 µm), and Molinari et al. (2008) (850 µm). The contours in the bottom right panel are the map of the 3.6 cm continuum emission observed by Molinari et al. (2002), while the ellipse in the bottom right denotes the corresponding angular resolution. The circle in the bottom left of each panel represents the HPBW of the corresponding image.


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

star observed for calibration during the night was saturated in all frames. Thus, we calibrated our photometry on 2MASS, by matching our sources to 2MASS PSC entries. For both bands, the colour range spanned by the common stars is too narrow to clearly show any colour effects between our instrumental magnitudes and 2MASS magnitudes, so we neglected colour terms. We obtained Ks (2MASS) - Ks (instrumental) = 23.81 ± 0.06 and H (2MASS) - H (instrumental) = 24.52 ± 0.05. The limiting magnitudes (at 3) are Ks 20 and H 20.5. A simple method of estimating the photometric completeness limits relies on histograms of magnitudes. Typically, the number of sources retrieved increases with increasing magnitudes up to a maximum value. Beyond this value, the source statistics is dominated by the decreasing efficiency in retrieving faint sources. Thus, the histogram maximum yields a rough estimate of the completeness limit. We conservatively assumed it to be 1 magnitude brighter than the histogram maximum. In fact, we found two nearby peaks at H , but the brighter one disappears when counting only sources in the 2 innermost part of the image. So the brighter peak is probably due to including sources from parts of the image with lower signal-to-noise ratio. The completeness limits we estimated are K s(compl) 17.75 and H (compl) 18.25. Finally, we calibrated the line emission fluxes on the final averaged (mosaiced) H2 image by repeating our photometry on the H2 image and matching it to the Ks calibrated photometry, correcting the stellar fluxes to the c of the narrow-band filter. Photometry of the H2 knots was then performed on the continuum-subtracted H2 images by means of task POLYPHOT in IRAF, enclosing each knot with polygons following the emission contour at 3 of the background counts as closely as possible. The identified knots and corresponding fluxes are given in Tables A.2 to A.4, where we have classified the knots on the basis of their association with Jet 1, Jet 2, and Jet 3 (defined in Sect. 3.3). For the H2 images the 3 sensitivity level is equal to 4 â 10-16 erg s-1 cm-1 arcsec-2 .
2.1.2. Near-IR images with FLAO and the PISCES camera

66 sources with detection both at Ks and H , 83 sources with detection at Ks , and 24 sources with detection at H (see Table A.5). We used aperture radii of 1 PSF-FWHM and annuli with inner and outer radii of 2­4 PSF-FWHM to derive the sky level, with the median as an estimator. We calibrated Ks and H by comparing the instrumental magnitudes to those obtained with LUCI (which in turn are calibrated on 2MASS) for the matching stars. Again, the colour range spanned by the data points is too narrow to show any clear colour effects, so we neglected colour terms. We obtained Ks (LUCI, 2MASS) - Ks (PISCES, instrumental) = 23.46 ± 0.10 and H (LUCI, 2MASS) - H (PISCES, instrumental) = 24.68 ± 0.11. We note that a few points depart by up to 0.4 mag from these relations. The most extreme differences are clearly due to unresolved objects in the LUCI images. Nevertheless, part of the scatter is probably due to PSF variations over the PISCES field (anisoplanatism), which is typical of AO-assisted images (e. g., Esslinger & Edmunds 1998). So, we can actually expect intrinsic errors of up to 0.1­0.2 mag in our PISCES photometry. The limiting magnitudes (at 3) are Ks 22.5 and H 21. We estimated the completeness limits as explained in Sect. 2.1.1. The distribution of Ks displays two nearby peaks (see Sect. 4.1), but the brightest one is likely to be intrinsic to the local stellar population. Thus, we derived Ks (completeness) 19.25 and H (completeness) 18.75. Finally, from the Ks and H2 images we obtained a continuum-free, pure H2 line emission map following the method described in Sect. 2.1.1.
2.2. Ground based mid-IR observations

The data were collected on October 9 and 12, 2013, using the PISCES Near Infrared Camera (McCarthy et al. 2001) installed at the focal plane of the First Light Adaptive Optics system (Esposito et al. 2010, 2011) of the Large Binocular Telescope. The detector has a pixel scale of 0. 02, with a field of view of 21 â21 . The observations were carried out through the H2 , H , and Ks filters. We used a star 10 west from our field center with R, I mag 12.0 as the reference for the AO loop, closed using 153 modes. The average Strehl Ratio on the centre of the field was 40% being measured on the H2 images. The electronic cross-talk between the quadrants in the PISCES Hawaii-I detector was corrected for each frame using Corquad, an IRAF procedure developed by Roelof de Jong2 . We obtained one image per band by registering and combining together, after sky subtraction: 119 exposures of 5 s at Ks (total integration time 595 s); 62 exposures of 25 s at H2 (total integration time 1550 s); and 3 exposures of 10 s at H (30 s). Due to the deteriorating weather conditions, only the latter small set of H frames is available. Each single frame was first drizzled, bad-pixel corrected, and flat fielded using standard IRAF routines. The PSF-FWHMs we measured are 0. 08 in all final images. We performed aperture photometry on the PISCES final images by using the DAOPHOT routines in IRAF. We found
2

See http://66.194.178.32/rfinn/pisces.html

Ground-based diffraction-limited mid-infrared images at 8.9, 9.9, 12.7, and 18.7 µm of IRAS 05137+3919 were taken on the night of November 9, 2006 with the mid-infrared camera CID (Salas et al. 2006) mounted on the 2.1 m telescope of the ´ ´ Observatorio Astronomico Nacional at San Pedro Martir, Baja California, Mexico. This camera is equipped with a Rockwell 128â128 square pixel Si:As BIB detector array that delivers an effective scale of 0. 55/pixel covering a fully-sampled area of 62 â62 . The images were taken with the standard chopnodding mode to remove the sky and telescope emission background. The standard stars Lyr, And, Aur, Her, and Aqu were observed before and after the programme sources at similar air masses for flux calibration, following Salas et al. (2006), in order to measure the PSF at each wavelength. These values (FWHM) ranged from 1.7 at the shortest wavelength, to 2. 1 at 18.7 µm. Individual images were obtained at ten nodding positions, 20 apart, while we chopped at 3 Hz with a throw of 22 . After all cycles, the total on-source integration time in each filter was 1440 sec. The astrometry of the images was determined by alignment with WISE and Spitzer/IRAC images. For this purpose, we smoothed the 8.9 and 9.8 µm images to 2 resolution and overlaid them by eye on the 4.5 µm IRAC image. The same procedure was adopted for the 12.7 and 18.7 µm images, which were compared to the 12 µm WISE image after smoothing them to 6. 5 resolution. Albeit not very accurate, this method results in an astrometrical error <1 , which will suffice for our purposes. A single mid-IR source was detected at all wavelengths. At < 13 µm, the source may be slightly resolved, with diameters >2 . The measured photometry on the CID calibrated images with a 4 aperture yields the following fluxes: 1.2 Jy at 8.9 µm, 1.5 Jy at 9.9 µm, 3.8 Jy at 12.7 µm, and 10.7 Jy at 18.7 µm. These values have 10% errors, dominated by uncertainties in the flux calibrations on standard stars as discussed by Salas et al. (2006).


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

5

2.3. IRAM 30-m telescope

The observations were performed with the IRAM 30-m antenna on Pico Veleta (Spain) on July 13 and 14, 2003. The source was mapped with HERA, a multi-beam heterodyne dual polarization receiver, consisting of two arrays of 3â3 pixels with 24 spacing (Schuster et al. 2004). Areas of 4 â4 and 3 â3 centred around the position (J2000)=05h 17m 13s.8, (J2000)=39 22 20 were covered, respectively, in the 12 CO and C18 O J =21 rotational transitions. The maps were made in on-the-fly mode, scanning along the right ascension direction. The receiver was suitably rotated to allow for a sampling with 4 intervals in declination, perpendicular to the scanning direction, while the data were acquired along the scanning direction every 4 . This results in excellent sampling of the 12 halfpower beam width (HPBW) of the telescope. Position switch and frequency switch were used, respectively, for the 12 CO(2­ 1) and C18 O(2­1) line observations. The VESPA autocorrelator was chosen as a backend, with a spectral resolution of 0.1 km s-1 and 0.053 km s-1 , respectively, for the 12 CO and C18 O(2­1) lines. The pointing accuracy was regularly checked (typically every hour) on strong, pointlike continuum sources. The data presented in this paper are expressed in main beam brightness temperature, T MB , assuming a forward efficiency of 0.90 and a beam efficiency of 0.52 for 12 CO(2­1) and 0.55 for C18 O(2­1). The conversion to flux density, S , is given by the expression S (Jy) = 4.7 T MB (K). The data were reduced and analysed by means of the GILDAS software3 . The spectra were smoothed to 0.5 km s-1 before creating channel maps of the line emission.

3. Results
The observational findings of our study are illustrated in the following, where we concentrate on four main issues: the largescale structure, extending over 100 , or 4 pc, around the nominal position of IRAS 05137+3919 ­ (J2000)=05h 17m 13s.3, (J2000)=39 22 14 ; the small-scale structure, namely the region of <20 , or <0.8 pc, imaged with the PISCES camera; the jets and corresponding outflows (hereafter "jets/outflows") mapped both in the near-IR and at 3.4 mm; and the stellar clusters, spread over 2 .
3.1. The large-scale structure

For the sake of simplicity, in the following we refer to the northern clump and associated cluster (hereafter "clump/cluster") as C1, to the southern clump/cluster as C2, and to the south-eastern cluster as C3 (see the top, right panel of Fig. 1). C1, which is the target of our investigation, is by far the most luminous at all frequencies and is the only one where freefree emission has been detected by Molinari et al. (2002), as one can see from the contour map in Fig. 1. The richness of C1 is illustrated also in the left panel of Fig. 2, where a 3-colour image of the whole region obtained from the LUCI data is shown. Here, the presence of the three clusters C1, C2, and C3 stands out clear (white colour), as well as the existence of multiple H2 jets (red colour), which we will discuss in the following. Thanks to the Hi-GAL images, it is now possible to obtain an accurate estimate of the far-IR flux densities and hence of the luminosities of C1 and C2. We reconstructed the corresponding spectral energy distributions (SEDs) using data from the 2MASS (Skrutskie et al. 2006), Spitzer/IRAC (Werner et al. 2004; Fazio et al. 2004), IRAS, MSX (Price et al. 1999), WISE (Wright et al. 2010) archives, the Herschel/Hi-GAL survey, the SCUBA Legacy Surveys (Di Francesco et al. 2008), and the studies of Molinari et al. (2008) and Ishii et al. (1998). When possible, the flux densities were taken from the available source catalogues. In the other cases, for each clump we integrated the continuum flux inside a suitable polygon enshrouding all the emitting region, and then subtracted the background estimated through 1-D cuts across the clump centre. The flux densities computed in this way, as well as the solid angles encompassed by the polygons used for the integration are given in Table A.6, while the corresponding SEDs are shown in Fig. 3. The bolometric luminosity was estimated by integrating the SED over the whole wavelength range, after linear interpolation in the Log­LogS plot. For the fiducial distance of 8.3 kpc we obtain 2.4 â 104 L for C1 and 6.7 â 103 L for C2. These numbers agree within a factor 2 with the estimates obtained from the cluster simulations of Faustini et al. (2009) and Kumar et al. (2006), once the different distance assumed in their calculations (11.5 kpc) is taken into account.
3.2. The small-scale structure

As already noted by various authors, two molecular clumps are detected in the IRAS 05137+3919 region, offset by 30 along the N­S direction. In this study we focus on the northern one, but it is worth mentioning that the two clumps are likely physically close in space and not only in projection onto the plane of the sky, because their LSR velocities differ by only 1 km s-1 (see Brand et al. 2001). Each of them hosts a stellar cluster, as pointed out by Faustini et al. (2009). In Fig. 1 we show a number of maps of the continuum emission of IRAS 05137+3919, ranging from the near-IR to the submm. We have chosen the images with the best angular resolution available in each wavelength regime. Besides confirming the previous findings, the IR images clearly indicate the existence of a third stellar cluster, located 15 to the east of the southern clump and considerably fainter than the other two clusters, which are dominating the emission at all wavelengths.
The GILDAS software has been developed at IRAM and Observatoire de Grenoble ­ see http://www.iram.fr/IRAMFR/GILDAS
3

As explained in Sect. 2, with the LBT/PISCES imaging we have attained a resolution of 80 mas or 664 au over 20 . This allows us to investigate in detail the innermost region of C1, which is the target of the present study. Our findings are best illustrated by the 3-colour image in the right panel of Fig. 2, where several features are worth of mention. The "white" star to the west of the image, is very likely a foreground object, not physically related to the cluster of interest for us. The two "yellow" stars at the centre are well separated, with the one to the NE (hereafter A, after Varricatt et al. 2010) appearing slightly "redder" and hence more extincted than the other (hereafter B). While the presence of this pair was already known, in our image A splits into two sources, one, brighter, to the SW (which we call A1) and another, fainter, to the NE (A2). This is more evident in Fig. 4, where we compare the LUCI to the PISCES images. Clearly, the dramatic improvement in angular resolution obtained with AO is crucial to resolve A1 from A2, whose apparent separation is 0. 18 (i.e. 1500 au). All three sources, A1+A2+B, are likely responsible for the ´ mid-IR emission measured by us with the San Pedro Martir telescope, as demonstrated by Fig. 5, where we overlay the LUCI Ks image on the four images at wavelengths ranging from 8.9 to 18.7 µm. Despite the limited astrometrical accuracy (1 ), it is


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Fig. 2. Composite colour images obtained by combining the emission in the H2 (red), Ks (green), and H (blue) filters from the LUCI (left panel) and PISCES (right panel) data. The dashed box in the left panel indicates the region shown in the right panel. The LUCI and PISCES images cover regions, respectively, of about 0. 8â1. 1 and 0. 3â0. 4.

Fig. 3. Spectral energy distributions of clumps/clusters C1 (left panel) and C2 (right panel). The colour coding of the symbols is explained in the left panel. The triangles indicate upper limits.

clear that the bulk of the mid-IR emission arise from the same region where the near-IR emission peaks. In turn, this implies that the three sources are responsible for most of the luminosity estimated for C1 (2.4 â 104 L ), because their mid-IR emission at 12.7 and 18.7 µm corresponds to 80% of the flux densities measured within much greater HPBWs with MSX and WISE (see Table A.6).

An interesting feature seen in Fig. 2 is the "green" arc of continuum emission extending to the SW from B. This almost coincides with three H2 knots, which can be recognised from their red colour in the image. Whether the arc and the knots are physically related is difficult to establish, but it is possible that both are manifestations of the same phenomenon, perhaps a bow shock due to Jet 1. In any case, the knots are in all likelihood due to the interaction between the jet and the dense gas associated


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

7

Fig. 4. Images of the central region of clump/cluster C1, where a pair of bright stars (A and B) had been detected in previous studies. The left and right panels refer, respectively, to Ks and H band images, while the upper and lower panels show, respectively, images obtained with the LUCI and PISCES+AO cameras. The values of the contour levels are indicated by marks in the corresponding colour scales. Note how employing AO allows us to resolve star A into the two sources A1 and A2.

with C1. As explained in Sect. 1, Jet 1 was first observed by Varricat et al. (2010) and is confirmed by our images (see below). Finally, at the top and bottom of the right panel of Fig. 2, one sees two other "red" regions of H2 line emission, shaped like bow shocks. These correspond to (part of) Jet 2, also identified by Varricat et al. (2010).
3.3. The bipolar jets/outflows

Evidence for the existence of multiple jets/outflows in the IRAS 05137+3919 region has been provided by various studies, as described in Sect. 1. Our high-resolution images shed new light on this issue, thanks to their superior sensitivity and angular resolution. Moreover, the velocity information conveyed by the 12 CO maps makes it possible to discriminate between the blueand red-shifted lobes. In Fig. 6, maps of the outflow lobes are shown, obtained by integrating the 12 CO(2­1) emission over the line wings, in various velocity intervals. These maps are compared to the H2 images obtained with LUCI, which fully confirm the existence of two bipolar jets associated with C1. The left panel of Fig. 6 displays the high-velocity (HV) emission, which nicely coincides with Jet 2 and indicates that this jet likely lies close to the plane of the sky, because the red and blue lobes overlap significantly. The low-velocity (LV) maps shown

in the right panel of the same figure look more complicate. In this case, the 12 CO emission appears to be consistent with Jet 1, but significant blue-shifted emission is seen towards the red lobe, whereas no red-shifted emission is detected over the blue lobe. The complex pattern observed may be due to confusion between the LV gas and that moving at the systemic velocity (whereas such a confusion obviously cannot occur for the gas that expands at high speed in Jet 2). Also, one has to take into account that the blue-shifted emission to the SW might be partly contaminated by the bulk emission from C2 (see Sect. 3.1), whose systemic velocity differs by ­1 km s-1 from that of C1. Incidentally, we note that the C1 and C2 clumps are also traced by the C18 O(2­1) line map ­ shown in the middle panel of Fig. 6. Despite the previous caveats, we conclude that in all likelihood the LV 12 CO outflow is related to Jet 1, while the HV 12 CO outflow is associated with Jet 2. A new feature that can be seen in our image is the presence of elongated H2 line emission originating approximately from the peak of the C18 O map (see Fig. 6) and extending towards W-SW over 4 . Clearly, this feature cannot be related to Jet 2, as the two are roughly perpendicular to each other. As for Jet 1, its SW lobe spans position angles (PA) between ­179 and ­ 145 (see the bow-shock shaped H2 knots spread over a region of 30 ), quite different from that of the new H2 feature (PA­


8

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

´ Fig. 5. Map of the LUCI Ks image (contours) overlaid on the mid-IR images acquired with the San Pedro Martir 2.1 m telescope. stars (A and B) had been detected in previous studies. The wavelength of each image is indicated in the top right of the panels, while the FWHM of the PSF is drawn in the bottom left. Note that all mid-IR images have been smoothed to the resolution of the 18.7 µm image.

118 ). We conclude that such a feature might be a third, smallscale jet previously unobserved and in the following we refer to this as Jet 3. The nature of Jet 3 will be better discussed in Sect. 4.3.
3.4. The stellar clusters

Some properties of the stellar population associated with cluster C1 can be derived from the colour-magnitude diagram of Fig. 7, where the LUCI and PISCES photometry are overlaid. The much smaller field imaged with PISCES is less contaminated by foreground field stars and allows us to characterise the colour spread of the cluster members. While the LUCI data points are distributed along a stripe close to the zero-age main sequence (ZAMS), with a number of very extincted sources (up to AV 40), the PISCES data points spread redwards of the stripe. The typical reddening of the cluster members can then be derived by reddening the ZAMS up to the nearest envelope of the PISCES data-point distribution, yielding AV = 5. Thus, the LUCI sources close to the ZAMS are essentially foreground field stars, whereas the cluster members are distributed with AV > 5 from the ZAMS (H - Ks > 0.4). In principle, the colour spread of the cluster members could be produced by extinction varying in the range AV 5­ 40. However, the colour­colour diagram ( J ­H vs H ­Ks ) of

Nikoghosyan & Azatyan (2014) displays a large fraction of stellar sources with near-IR colour excess. This excess is usually caused by the presence of disks around young stars. By incorporating theoretical accreting disk models, their effect on the Ks versus H ­Ks diagram has been demonstrated for disks around T Tauri stars to be accurately represented by vectors of approx´ imately constant slope (Lopez Chico & Salas 2007), towards brighter Ks and redder H ­Ks values. More massive YSOs are usually much more embedded than T Tauri stars, and the cor´ rection proposed by Lopez Chico & Salas (2007) is unlikely to apply to such objects. However, the presence of a spherical envelope around the disk should cause a greater decrease of H ­Ks for the same variation of Ks , than in the case of a "naked" disk. ´ Therefore, one can use the Lopez Chico & Salas (2007) correction to obtain a lower limit to the spectral type. Assuming reddening along the arrow in the bottom of Fig. 7, after dereddening the three objects for a minimum interstellar extinction of AV =5, one obtains spectral types of B7 for A1 and A2, and B1 for B. Vice versa, assuming that only interstellar extinction is responsible for the reddening, along the arrow drawn in the top of Fig. 7, one estimates spectral types earlier than O8 for all three sources. The constraints set by this method on the stellar type are quite loose, but consistent with the three objects being intermediate- to high-mass stars.


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9

Fig. 6. Left. IRAM 30-m maps obtained by averaging the 12 CO(2­1) over the HV line wings, overlaid on the H2 line (i.e. continuum subtracted) emission image obtained with LUCI. The integration has been performed over the LSR velocity intervals ­35.65,­32.65 km s-1 (blue contours) and ­17.65,­14.65 km s-1 (red contours). Contour levels range from 0.8 to 4.16 in steps of 0.48 K. The circle in the bottom left denotes the HPBW of the 30-m telescope. Right. Same as left panel, for the 12 CO(2­1) LV wing emission. The integration was performed over the intervals ­29.65,­27.65 km s-1 (blue contours) and ­22.65,­20.65 km s-1 (red contours). Contour levels range from 1.2 to 15.6 in steps of 1.44 K. Middle. Map of the C18 O(2­1) line emission averaged over the line, from ­27.65 to ­24.15 km s-1 . Contour levels range from 0.54 to 1.62 in steps of 0.36 K.

Incidentally, this also proves that A1, A2, and B are part of the same system and none of them is likely to be spurious. A contaminant field star could only be a background (due to its extinction), more distant, giant or supergiant star (due to its unreddened brightness), but the probability of such a luminous object lying in the same projected area of our system is very low.

4. Analysis and discussion
The purpose of the following sections is to tie the large to the small scale structures in IRAS 05137+3919, and thus identify the sources powering the jets/outflows and establish their nature.

4.1. Characterization of the stellar population

Using the extinction estimated from the colour-magnitude diagram, we can convert our Ks completeness limits into stellar mass limits. Assuming AV = 5, a cluster age of 1 Myr, a distance of 8.3 kpc, and adopting the pre-main sequence tracks of Palla & Stahler (1999), we obtain a mass completeness limit of 0.5 M with the LUCI photometry and 0.1 M with the PISCES photometry. For more extincted stars the completeness mass increases; e.g. AV =20 yields 2.0 M with the LUCI photometry and 0.7 M with the PISCES photometry. However, we note that these values refer to "naked" stars. On the other hand, stars exhibiting a near-IR excess shine brighter at Ks , as already said, and the effective mass completeness limit decreases. The assumed age is consistent with that derived by Faustini et al. (2009), and the extinction values at the cluster peaks (derived from the sub-mm emission) listed by those authors towards C1 (AV = 18) and C2 (AV = 8) lie inside our adopted range. We also note that our Ks completeness limits are 1 mag (LUCI) and 2.5 mag (PISCES) less than achieved by Faustini et al. (2009), allowing us to improve on their results. A detailed analysis of the cluster stellar population will be presented in Sect. 4.1.

A problem with young stellar clusters, especially those as distant as IRAS 05137+3919, is that their central areas are dominated by diffuse emission, source crowding, and the wings of the PSF of the brightest stars, which lead to a local worsening of the photometric completeness limit. In turn, this biases the derived properties (e. g., cluster density profile, number of members, etc.). We can assess this effect towards IRAS 05137+3919, by comparing the histograms of Ks PISCES sources and LUCI sources inside the field imaged by PISCES. These are shown in Fig. 8. We adopted a bin width of 0.5 mag, larger than the maximum uncertainty on the PISCES photometry. Clearly, the LUCI histogram peak is brighter than the LUCI completeness limit estimated all over the LUCI field of view. In addition, the number of Ks sources brighter than the completeness limit and retrieved with LUCI is less than those detected with PISCES. An interesting characteristic of the PISCES histogram is its double peak. While the fainter peak is due to increasing incompleteness in sampling the stellar background population, the brighter peak is very likely an intrinsic feature of the C1 cluster population, as


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Fig. 8. Histograms of the distribution of Ks source magnitudes inside the field of view of PISCES. The red solid line indicates PISCES sources, the black dashed one LUCI sources. The vertical black and red dotted lines show, respectively, the completeness limit of the LUCI and PISCES Ks photometries, estimated from the whole corresponding field (see text).

Fig. 7. Ks vs H ­Ks diagram of the sources retrieved in the LUCI field (black squares) and in the PISCES field (red squares). The dashed lines shows the completeness limit of the LUCI photometry (black) and the PISCES photometry (red). The black solid line is the ZAMS at a distance of 8.3 kpc (derived using the colours of Koornneef 1983 and the absolute magnitudes of Allen 1976 and Panagia 1973). The position of a few spectral types is labelled. The arrow in the top shows the effects of an extinction of AV =20 (according to Rieke & Lebofsky 1985). The arrow in the bottom corresponds to the median disk excess vector of ´ Lopez-Chico & Salas (2007) for the accretion disk models of D'Alessio et al. (2005). The three brightest members of the cluster C1 are labelled, as well. Fig. 9. Surface radial density of Ks sources derived in concentric annuli centred at the position of B, the brightest cluster member. The solid line indicates the density as computed from the LUCI photometry. The dashed line indicates the density computed by replacing the LUCI photometry with the PISCES photometry inside the area corresponding to the field of view of PISCES. The sources are counted up to the LUCI completeness limit (i.e. Ks 17.75). The errorbars show the Poissonian count fluctuations.

it lies well above the completeness limit of PISCES (red dotted line in Fig. 8). How much the degraded completeness limit in the innermost, densest part of C1 affects the observed cluster properties can be assessed by plotting the surface radial density of Ks sources as derived in concentric annuli centered at the brightest cluster member (i.e. B). As shown in Fig. 9, when the LUCI sources are replaced by the PISCES ones inside the field of view of PISCES (and only counting sources with Ks 17.75, the LUCI completeness limit), the surface density doubles at the centre. The outermost annuli give an approximate measure of the field star density, which may be subtracted from the central peak to derive the real stellar density of cluster C1. Note that the density plateau between 1 pc and 2 pc is due to the small clusters C2 and C3, rather than to a halo of members around C1. The number of cluster members can be derived from the radial surface density distribution in Fig. 9 like the "richness indicator" Ic (see e.g. Testi et al. 1998). This implies integrating on the inner annuli and using the outermost annuli to estimate

the background correction. We have integrated up to a radius of 0.97 pc and 1.93 pc to obtain, respectively, the total richness indicators for C1 (Ic = 87 ± 2 stars) and C1+C2+C3 (Ic = 120 ± 4 stars). For this purpose, we used the radial surface density corrected with the PISCES photometry (dashed line in figure). We note that Ic is much larger than obtained by Faustini et al. (2009), due both to our crowdness correction and more sensitive completeness limit. Our estimate of 87 stars pc-2 seems comparable to the values derived by Testi et al. (1999) for their sample of Herbig Be stars. However, one must take into account that their sensitivity is better than ours by a couple of magnitudes at Ks , af-


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

11

ter suitable scaling for the smaller distance of their targets (less than 1 kpc). Therefore, we may reasonably conclude that C1 is significantly richer than the clusters around Herbig Be stars. Once more, we speculate that this might be related to the age of the cluster, as ours is younger than those of Testi et al., being associated with molecular gas and powerful outflow activity. Finally, Ic can be converted into a total number of cluster members provided a suitable initial mass function (IMF) is assumed. However, such a conversion is hindered by the uncertainty on the mass completeness limit. The latter depends on the real distribution of the extinction, which we cannot derive from our data, and stellar age. We have quoted a mass completeness limit (corresponding to Ks = 17.75) between 0.5 and 2 M , but this should be further decreased if the cluster is younger than the adopted value of 1 Myr. In addition, in clusters that young, a high fraction of low-mass stars are still associated with a circumstellar disk and do exhibit a near-IR excess (see Sect. 3.4), which makes their detection easier. If we roughly assume that the Ic value is representative of >1 M stars, by considering a standard IMF (e.g. Scalo 1998), then the total number of C1+C2+C3 members (down to 0.1 M ) would be 700. In this case, the IMF would predict 2 members with M > 15 M . We conclude that our cluster analysis supports the existence of 2­3 early B-type stars, consistent with our estimates of the luminosities of sources A1, A2, and B.
4.2. Characterization of the jets/outflows

and 2. We thus believe it is very reasonable to assume that the YSOs powering these jets/outflows lie inside C1, and we will base all our reasoning on such an assumption. The left panel of Fig. 10 shows that the SW lobe of Jet 1 consists of a number of bow-shock-like features spread over a broad region, unlike the NE lobe, which appears well collimated. One may hence wonder whether Jet 1 is not a single jet, but the result of multiple jets overlapping in the plane of the sky. A priori, the H2 knots falling in the regions corresponding to clusters C2 and C3 might belong to small jets powered by stars of those two clusters. However, careful inspection of the H2 image reveals that all of the knots to the SW have bow-shock shapes pointing to the SSW, which is inconsistent with the driving source to be located in C2 or C3. We thus believe that in all likelihood these knots belong to Jet 1, whose origin lies in cluster C1. If this is the case, why does the SW lobe appear so much less collimated than the NE lobe? A possibility is that the two lobes are intrinsically similar, but the SW one looks wider because it is impinging against C2 and C3, where one sees H2 shocked emission. The NE lobe, in contrast, is expanding through lower density medium, which could confine the H2 emission to internal shocks along the jet axis (see e.g. Stone et al. 1997).
4.2.2. Jet 2

As H2 our Jet

illustrated in Sect. 3.3, evidence for the existence of up to 3 jets is seen in the IRAS 05137+3919 region. Here we focus analysis on the most prominent of these, namely Jet 1 and 2, and postpone the discussion of Jet 3 to Sect. 4.3.1.

4.2.1. Jet 1

While the existence of Jet 2 is out of question, due to its nice bipolar and well collimated morphology, the structure of Jet 1 is more complex and casts some doubts on the unicity of this jet. A priori, one might consider the possibility that the complex pattern of this jet might be due to precession. Although such a hypothesis cannot be ruled out, we prefer not to discuss it any further, because a precessing jet should describe an S-shaped pattern on the plane of the sky (see e.g. Fig. 18 of Cesaroni et al. 2005), while no convincing evidence of such a pattern is seen in our case. We thus attempt to explain the observed features with the simplest possible model, without invoking additional mechanisms besides expansion. Is it possible that Jet 1 is in fact the result of the combination of multiple, distinct jets? To investigate this issue and establish the origin of the jets, in Fig. 10 we compare our near-IR images with other IR and molecular line maps. In the left panel we show an overlay of the 4.5 µm Spitzer/IRAC map on the LUCI image of the H2 line emission. One sees that basically all of the H2 knots belonging to Jet 1 coincide with peaks of the 4.5 µm emission. This is consistent with the presence of unresolved H2 lines in the bandwidth covered by the Spitzer/IRAC 4.5 µm filter. The middle and right panels clearly illustrate the presence of three stellar clusters, already discussed in Sect. 3.1, traced by the low-resolution 3.4 µm WISE image and resolved in our 1.6 and 2.2 µm LUCI images. We also compare the near-IR emission to the HCO+ (1­0) interferometric map of Molinari et al. (2002), to show that the brightest cluster is associated with a dense molecular core in C1, and lies close to the geometrical centre of jets 1

Jet 2 looks much better defined than Jet 1 and is clearly centred on the peak of the molecular clump C1, as shown by the comparison with the HCO+ line emission (middle panel of Fig. 10). As already noted, the 12 CO(2­1) outflow appears to mirror the pattern of the H2 jet, thus allowing a kinematical analysis of the jet/outflow structure. For this purpose, we assume that the YSO powering this outflow coincides with one among A1, A2, and B. Evidence in favour of this hypothesis will be provided in Sect. 4.3. In Fig. 11 we show the position­velocity (PV) plot along the Jet 2 axis, namely for PA=­17 . While the LV emission (between ­30 km s-1 and ­22 km s-1 ) is confused by the extended 12 CO bulk emission close to the systemic velocity of -25 km s-1 (Brand et al. 2001), beyond this interval one sees both red- and blue-shifted emission, both at positive (10 ) and negative (­10 ) offsets. However, the mean velocity of the emission is slightly skewed to the red at positive offsets and to the blue at negative ones. We will demonstrate that such a difference can be explained by a (small) inclination of the outflow with respect to the plane of the sky. To prove our hypothesis and obtain an estimate of the inclination angle (important for a correct estimate of the outflow parameters), we have applied the conical outflow model of Cesaroni et al. (1999) to our case. This is a simple-minded model that assumes that the outflowing material is confined inside a cone with aperture angle , inclination angle with respect to the plane of the sky, length of each lobe R0 , and expansion velocity V = V0 (R/R0 ). The model computes the pattern inside which emission is expected in the PV plot. Reasonable guesses for the input parameters , , and V0 can be obtained by solving Eqs. (A6), (A7), and (A8) of Cesaroni et al. (1999). For this purpose, we need an estimate of the projection of on the plane of the sky, , and the maximum and minimum velocities along the line of sight (relative to the systemic velocity of ­25 km s-1 ) ob(1) (2) served in each lobe, Vz,max and Vz,min (in the notation of Cesaroni et al. 1999). The latter are obtained from Fig. 11 and are, respectively, 8.8 km s-1 and 7 km s-1 , while can be estimated from the jet/outflow maps in Fig. 6 and is about 15 ­30 . The solution of the three equations is 0 , 15 ­30 , and V0 16­


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Fig. 10. Left. Overlay of the 4.5 µm Spitzer/IRAC image (contours) on the LBT/LUCI image of the H2 line emission (continuum subtracted). Contours are drawn in 5 logarithmic steps from 1 to 60 MJy/sterad. The angular resolution of the contour maps is indicated by the circle in the bottom left. Middle. Same as left panel, for the overlay of the HCO+ (1­0) line OVRO map by Molinari et al. (2002), corrected for primary beam attenuation, on our LBT/LUCI Ks -filter image. The HCO+ map has been obtained by averaging the emission between ­28.76 and ­20.78 km s-1 . Contour levels range from 57 to 342 in steps of 95 mJy/beam. The dashed circle denotes the primary beam of the OVRO interferometer. Right. Same as left panel, for the overlay of the WISE 3.4 µm map on the LBT/LUCI H-filter image. Contours are drawn in 6 logarithmic steps from 1 to 76 MJy/sterad. Labels C1, C2, and C3 have the same meaning as in Fig 1.

31 km s-1 . Since the outflow axis lies very close to the plane of the sky, R0 can be obtained directly from the outflow maps and is 14 . The best fit was obtained by slightly varying the input values around these guesses. and is represented by the solid pattern in Fig. 11 (computed from Eq. A2 and A3 of Cesaroni et al. 1999), which corresponds to R0 = 14 , V0 = 30 km s-1 , = 15 , and = 2 . The model mimics the shape of the 12 CO emission quite well and proves that the outflow axis is indeed almost perpendicular to the line of sight. It is instructive to check how much the pattern would change for a slightly different inclination angle, e.g. = 10 . This is shown by the white, dashed lines in Fig. 11, which are significantly offset from the best fit. We thus conclude that the uncertainty on the inclination is very small. It is also useful to derive the main outflow parameters. These have been computed by integrating the 12 CO(2­1) line emission over the lobes, in the velocity intervals ­35.15,­29.65 km s-1 and ­21.15,­16.65 km s-1 . In the calculation we assume LTE at a temperature of 30 K, optically thin emission, and a 12 CO abundance relative to H2 of 10-4 . The resulting parameters have been divided by the outflow dynamical time scale tdyn = R0 /V0 0.56 pc/30 km s-1 1.8 â 104 yr, to obtain the mass loss rate, M = 4.2 â 10-4 M yr-1 , and momentum rate 9.2 â 10-3 M km s-1 yr-1 . The latter has been corrected P for the inclination of the flow with respect to the line of sight, assuming the outflow model described above. From P one can estimate the bolometric luminosity (L) of the source powering the outflow by means of the relationship between Log(P) and

LogL derived by Wu et al. (2004). From their Fig. 7 one obtains L 3 â 104 L , but with a large uncertainty which allows for values ranging from 103 L to almost 106 L . While this result does not permit us to set tight constraints on the nature of the YSO powering Jet 2, it is consistent with the bolometric luminosity estimate (2.4 â 104 L ) obtained from the SED (see Sect. 3.1) and confirms that one is indeed dealing with a high-mass star.
4.3. Identification of the sources driving the jets

Until now, we have assumed that the YSOs powering the jets/outflows in IRAS 05137+3919 are located close to the centre of the cluster shown in Fig. 2. Here, we want to prove that the origin of the jets/outflows is to be searched among the three brightest sources: A1, A2, and B. For this purpose, in Fig. 12 we present three images of the H2 jets, which progressively zoom into the neighbourhood of the three objects. For the sake of comparison, we also draw the borders of the conical jet model described in Sect. 4.2.2 (short-dash blue lines), centred on the position of B. This looks like an obvious choice, because star B lies right along the symmetry axis of Jet 2, unlike A1 and A2. Moreover, if the origin of the flow were shifted along that axis, the model in Fig. 11 could not reproduce the blue-red symmetry of the observed PV plot. Although one cannot rule out the possibility that another deeply embedded, yet undetected star within a couple of arcsec from B is powering Jet 2, this appears quite unlikely for the following reason. A1, A2, and B lie at the very peak of the molecular line and mm continuum emission, where


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13

Fig. 11. Position­velocity plot of the 12 CO(2­1) line emission along the direction matching the axis of Jet 2, i.e. with PA=­17 . The values of the contour levels are shown in the colour scale at the top of the figure. The offset is measured from an arbitrary position. The vertical and horizontal dashed lines indicate, respectively, the position of stars A+B and the systemic velocity of the associated clump. The white solid pattern encloses the region inside which emission is expected for the conical jet model that best fits the data (see text). The dashed pattern corresponds to the same model with a slightly different inclination angle (10 instead of 2 ; see text).

the column density should be highest (see Fig. 13). Despite this fact, all of them have been detected in our images, even at H band, which makes it difficult to believe that any other similar (or more luminous) star in the neighbourhood, where the column density is lower, could be so embedded to be undetectable. We thus conclude that star B is likely to be powering Jet 2. In Fig. 12, we also draw a tentative pattern for Jet 1 (red long-dash lines), under the working hypothesis that this originates from A1 or A2. The aperture angle of the jet is greater than for Jet 1 (20 ), consistent with the 12 CO outflow map in Fig. 6. In Fig. 13 one sees that the peak of the 3.6 cm continuum emission (Molinari et al. 2002) is roughly consistent with the position of A1/A2, with a tail of emission extending to the NE, in the direction of Jet 1. This alignment suggests that at least part of the free-free emission could originate from a thermal jet tracing the root of Jet 1. The most direct evidence for a tight association between A1/A2 and Jet 1 is presented in the right panel of Fig. 12, where we plot the relative proper motions of the H2 O masers observed by Honma et al. (2011). These are

clearly expanding along the Jet 1 axis, from a centre whose position is compatible (within the astrometrical uncertainty of the IR images) with that of the A1/A2 pair. Since water masers are believed to form in shocks, the observed association indicates that the maser motions are tracing the innermost part of the jet. This result casts some doubt on the interpretation of A1 and A2 as a binary system. Since the two objects are aligned along the Jet 1 axis, one should consider the possibility that they are the lobes of a small bipolar reflection nebula. Such an interpretation is supported by a comparison in the PISCES Ks image between the shapes of A1 and A2, on the one hand, and B, on the other hand. While the latter appears approximately circular, A1 and A2 are slightly elongated, respectively, in the E­W and N­S directions. Since the separations of the sources from the guide star are similar, the different shapes are unlikely to be due to anisoplanatism. We used DAOPHOT in IRAF to compare the PSFs by performing some experiments on the Ks image. We found that when using B as the reference PSF, after PSF subtraction through a fit, both A1 and A2 are oversubtracted, consistent


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Fig. 12. Left. LUCI image of the H2 line emission (continuum subtracted) tracing the jets in IRAS 05137+3919. The artefact due to continuum subtraction at the position of stars A1, A2, and B has been blanked (white area). The contours are a map of the continuum emission measured in the Ks filter. The contour levels have been chosen to show only the brightest stars in the field. The red long-dash and blue short-dash lines indicate, respectively, the borders of Jet 1 and Jet 2. Middle. Same as left panel, for a smaller region centred on the jets' origin. Right. Same as left panel, for a comparison between the H2 line and Ks continuum images taken with LUCI (top) and PISCES (bottom). The red points and corresponding arrows denote the H2 O maser spots and associated relative proper motions measured by Honma et al. (2011).

with them being slightly more extended. Moreover, when using A2 as the reference PSF, after subtraction A1 is still oversubtracted, whereas B is now undersubtracted, consistent with A1 being slightly more extended than A2. In summary, the PSFs of A1 and A2 differ from each other and that of A1 departs the most from a stellar PSF. In the light of the previous results, it seems plausible that A1 and A2 are not point-like stars but the marginally resolved lobes of a bipolar reflection nebula. In this case, the dark lane between the lobes could be due to a circumstellar disk, with size on the order of the separation between A1 and A2, namely 1500 au. This value is similar to the diameter of disks around high-mass (proto)stars (see Cesaroni et al. 2007). Note that the distance between the two maser spots is 1120 au, slightly less than the separation A1­A2, in agreement with a scenario where the masers trace the expansion of the jet in the densest part of it, closer to the star than the IR lobes, as observed in other similar objects (e.g. the massive protostar IRAS 20126+4104; see Cesaroni et al. 2013). We note also that the brightest source, A2, lies to the SW, namely in the direction of the blue-shifted lobe of jet1, consistent with the expectation that the brighter lobe of a reflection nebula is the one pointing to the observer. In conclusion, one should seriously consider the possibility that the pair A1/A2 is not a binary system, but a bipolar nebula associated with a disk+jet system from a massive star.
4.3.1. Jet 3

of 3 knots, with the northernmost of these lying 1 to the south of A1/A2. This structure suggests that one might indeed be observing a jet originating from another (lower-mass) star beside A1, A2, and B. However, in the high resolution image the first knot to the E disappears, whereas the others are still visible albeit partly resolved out. In our opinion, this indicates that the northern knot is an artefact due to residuals in the subtraction of the Ks continuum from the H2 filter, in the LUCI images. If this is the case, the other knots could be associated with Jet 1. In conclusion, while the presence of a third jet from another (possibly low-mass) YSO in the cluster cannot be excluded, we prefer to consider the simplest possible scenario, where all H2 knots are explained with only two jets (Jet 1 and Jet 2). Only future, more sensitive images of the jet/outflow structure could help us to establish the correct interpretation.
4.4. Nature of A1/A2 and B

Finally, we investigate the nature of (putative) Jet 3. The right panel of Fig. 12 shows an enlargement of it, with a comparison between the LUCI and PISCES images. At lower angular resolution the H2 emission seems to trace an elongated lobe, made out

The luminosity measured in Sect. 3.1 sets an upper limit of 2.4 â 104 L to that of the most massive member of cluster C1. There is little doubt that the luminosity must be dominated by A1/A2 and B, as these are by far the brightest sources in the field, with A2 being the brightest at Ks band (11.2 mag) and the one with the largest colour index (H ­Ks =3.8 mag). We deduce that the corresponding star is the most massive in the cluster, no matter whether A2 is a real star or the lobe of a reflection nebula. Actually, in the latter case, one would see only part of the photons emitted by the embedded star, thus lending further support to our previous statement that this is the most massive member of cluster C1. When discussing the luminosity of C1, is worth taking into account the inclination of the jets with respect to the line of sight.


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

15

Fig. 13. Left. Overlay of the contour map of the HCO+ (1­0) line (from Molinari et al. 2002) obtained by averaging the emission between ­27.08 and ­23.72 km s-1 , on the H2 line (i.e. continuum subtracted) LUCI image. Contour levels range from 150 to 420 in steps of 90 mJy/beam. Like in Fig. 12, the area around stars A1, A2, and B has been blanked to mask an artefact caused by the continuum-subtraction process. Middle. Overlay of the contour map of the 3.4 mm continuum emission (from Molinari et al. 2002) on the 2.2 µm continuum LUCI image. Contour levels range from 2.64 to 4.4 in steps of 0.88 mJy/beam. Right. Overlay of the contour map of the 3.6 cm continuum emission (from Molinari et al. 2002) on the 2.2 µm continuum PISCES image. Contour levels range from 0.069 to 0.161 in steps of 0.023 mJy/beam.

We have seen that Jet 2 lies close to the plane of the sky. A similar conclusion is likely to hold also for Jet 1, if A1 and A2 are reflection nebulae, because if the jet axis were close to the line of sight the nebulosity associated with the red-shifted lobe would not be detected. It has been shown (see Fig. 10 of Whitney et al. 2003) that beaming of photons along the jet axis, the socalled "flashlight effect", may lead to an underestimate of the source luminosity by a factor 2 ­ or even more (see Zhang et al. 2013). We thus caution that the luminosity of C1 might be significantly greater than our previous estimate of 2.4 â 104 L . We have attempted a more precise estimate of the total luminosity of A1+A2+B by fitting only the 2MASS J , H , Ks , our 8.9­18.7 µm, and the L-band measurements by Ishii et al. (1998), with the on-line model fitter4 by Robitaille et al. (2013). The other fluxes in Fig. 3 were set as upper limits. In the calculations we have fixed the distance to 8.3 kpc and assumed an interstellar visual extinction AV < 5 (see Rowles & Frobrich 2013). Despite the loose constraints, the first 50 best-fit models span a relatively small range in luminosity, Lmod =(4.4­ 15)â103 L . Taken at face value, this implies that 38­82% of the luminosity of cluster C1 is due to the lower-mass members of it. A range of values for the maximum stellar mass among A1, A2, and B is obtained under the two opposite assumptions that either only one star is responsible for Lmod , or all three stars equally contribute to Lmod . Correspondingly, one obtains a range for the most massive star in the cluster of 8­15 M (see e.g. Diaz-Miller et al. 1998). Alternatively, the luminosity of the most massive star(s) can be derived from the radio continuum flux density, assuming that this originates from an optically thin HII region around an earlytype star. One can compute the stellar Lyman continuum emis4

sion, and hence the luminosity, as done by Molinari et al. (2002), who obtain a Lyman continuum photon rate of 2 â 1045 sec-1 (after scaling from their distance of 11.5 kpc to ours of 8.3 kpc), corresponding to a luminosity of 6 â 103 L and a stellar mass of 11 M . These numbers appear to agree quite well with our previous estimates; however one should keep in mind that the radio continuum emission could be due to a thermal jet rather than a photoionised HII region. Multi-wavelength radio maps with better angular resolution are needed to establish the nature of this emission. Finally, we attempt an estimate of the luminosity using the H2 line emission. Following Caratti o Garatti et al. (2006), one may relate L to the luminosity in the H2 line, LH2 , by means of the expression Log[LH2 (L )] = (0.58 ± 0.06) Log[L(L )] - (1.4 ± 0.06) which holds for jets associated with stars from 0.1 to 105 L (see Caratti o Garatti et al. 2013). We have computed LH2 following the recipe of Caratti o Garatti et al. (2006), namely integrating the emission over all H2 knots belonging to the jet and then multiplying by 10 to correct for the energy radiated in the other non-observed H2 transitions. A further correction for the interstellar extinction must be applied. The Robitaille model fit previously described corresponds to a range AV =1.2­ 2.9, which translates into a correction factor at the wavelength of the H2 filter (2.12 µm) of 10A2.12µm /2.5 = 1.13­1.35 (where we assume a ratio A2.12µm /AV = 0.112; see Rieke & Lebofsky 1985). From the LUCI H2 image we obtain LH2 7.4 L for Jet 1 and LH2 1.5 L for Jet 2, which imply, respectively, L 8 â 103 L and L 5 â 102 L . These values are in good agreement with the those previously obtained from the IR fluxes and free-free radio emission, and confirm that star B could be powering Jet 2, while Jet 1 could originate from A1+A2, the most massive star(s) in cluster C1.

see http://caravan.astro.wisc.edu/protostars/sedfitter.php


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

4.5. Structure and kinematics of the molecular core

The interferometric observations of Molinari et al. (2002) have established the presence of a compact molecular core, where stars A1+A2 and B seem to be embedded. It is interesting to investigate the structure and kinematics of this core in relationship to the observed jets and stars. In Fig. 13 we plot a map of the HCO+ (1­0) bulk emission (contours in the left panel) on the image of the H2 line emission. Note that the HCO+ map in this figure differs from that in the middle panel of Fig. 10 because the latter has been obtained by integrating the HCO+ emission over the whole line profile, whereas the former considers only a small range around the systemic velocity. The shape of the core appears elongated E­W, namely roughly perpendicular to Jet 1 and Jet 2. In Fig. 14 we analyse the velocity field of the core, through maps of the peak velocity and line full width at half maximum (FWHM). These parameters have been obtained with a Gaussian fit to the HCO+ line profile, pixel by pixel, over the whole region where HCO+ emission was detected above 5. A clear velocity gradient is present in the E­W direction, with A1, A2 and B lying at positions where the velocity equals the systemic velocity of ­25 km s-1 . The line FWHM is minimum to the E and W of the core, and attains its maximum to the N and S, approximately where the jets emerge from the core. This suggests that the core is significantly perturbed by the material expanding along those directions. The question is how to interpret the shift observed in the peak velocity. It is possible that such a shift is due to Jet 1, whose red­blue symmetry looks consistent with the direction joining the maximum (located to the NE) and minimum (to the SW) HCO+ peak velocities. However, maximum/minimum velocities are seen also to the SE/NW and looking at the whole velocity field one gets the impression that the mean velocity gradient is directed E­W rather than NE­SW. With this in mind, one is tempted to interpret the velocity gradient as rotation of the core about the jets' axes. Under this hypothesis, the mass needed to guarantee rotational equilibrium of an oblate core with angular diameter 8 and rotation velocity 2 km s-1 is 150 M . This may be compared with the mass of the core computed from the 3.4 mm continuum flux of 21 mJy (see Table 3 of Molinari et al. 2002). In our calculation we adopt a dust absorption coefficient of 0.01 cm2 g-1 at 1.3 mm (for a gasto-dust mass ratio of 100 and using the estimates of Ossenkopf & Henning 1994), scaling like - with =1, and a dust temperature of 60 K (estimated from the ratio of the NH3 (1,1) and (2,2) inversion transitions observed in the RMS survey5 (Lumsden et al. 2013). Under these assumptions we obtain 120 M , with a large error due to the uncertainty on the dust absorption coefficient and dust temperature. Nonetheless, the core mass is of the same order of magnitude as the dynamical mass, consistent with the hypothesis of a core in rotational equilibrium. Based on the above, one may speculate that the stellar cluster is the result of the fragmentation of a rotating core, yielding a couple of massive stars with (remnants of) circumstellar disks, whose observable manifestations are Jet 1 and Jet 2. Further interferometric observations of the dense molecular gas are required to lend support to the proposed scenario.

vestigate the complex jet structure and the associated stellar cluster(s). The dramatically improved sensitivity and resolution as well as the broad frequency coverage obtained by complementing our data with archival data, allow us to obtain a number of results: ­ We identify 3 stellar clusters (C1, C2 and C3) in the region, with the two richest ones being embedded in molecular clumps. ­ The luminosity of the richest cluster, C1, which contains the brightest stars, is 2.4 â 104 L , a value typical of early Btype stars. We indeed conclude that the most massive star in C1 has a mass of 8­15 M . ­ Employing adaptive optics, we resolve the densest part of cluster C1 thus significantly increasing the number of known cluster members with respect to previous estimates based on lower resolution images. In particular, we find that of the two brightest stars, A and B, previously identified, the first is actually made of two distinct sources that we name A1 and A2. ­ The stellar cluster C1 turns out to be richer and less concentrated than those observed by other authors around Herbig Be stars and we thus speculate that the difference could be due to an evolutionary effect. ­ We confirm the existence of (at least) 2 bipolar jets/outflows and demonstrate that they originate from C1. Using various approaches, we come to the conclusion that both jets must be powered by early B-type stars. ­ By comparing the geometry and velocity field of the jets/outflows to the properties and location of the stars, we propose that the smaller jet is powered by the more luminous and less embedded star B, whereas the largest jet originates from the pair A1+A2. ­ We speculate that A1+A2 could be a small bipolar nebula along the jet axis, outlining a disk of 103 au seen in silhouette. This hypothesis is supported by the fact that the molecular gas appears to rotate (although on a much larger scale of 0.2 pc) about the jet axis. Our findings demonstrate the potential of sub-arcsecond resolution in the near IR to investigate high-mass star forming regions and call for further imaging at (sub)millimetre wavelengths with comparable resolution to shed light on the circumstellar environment and its connection with the large-scale jets. To date, only the ALMA interferometer can resolve structures as small as 100 mas and thus allow one to study the gas kinematics and physical properties on scales <100 au in IRAS 05137+3919 and similar regions.
Acknowledgements. It is a pleasure to thank Francesca Bacciotti and Daniele Galli for instructive discussions on jets from YSOs. MT acknowledges support from UNAM/PAPIIT grant No. IN-101813. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This publication also makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

5. Summary and conclusions
We performed observations at near-IR, mid-IR, and millimetre wavelengths of the star forming region IRAS 05137+3919 to in5

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see http://rms.leeds.ac.uk/cgi-bin/public/RMS DATABASE.cgi


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Fig. 14. Left. Overlay of the H2 line (i.e. continuum subtracted) LUCI image (contours) on a map of the peak LSR velocity of the HCO+ (1­0) line observed by Molinari et al. (2002). The artefacts due to continuum subtraction in the H2 image have been blanked as already done in Fig. 12. The dashed lines represent the axes of Jet 1 and Jet 2, while the two black points indicate the positions of stars A1+A2 and B. Right. Same as left panel, for the HCO+ (1­0) line full width at half maximum.

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Appendix A: On-line material


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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Table A.1. Coordinates, magnitudes, and colour of the sources identified in the LUCI field. The symbol "--" indicates a non-detection. RA (hh mm ss) 05 17 08.27 05 17 17.36 05 17 04.02 05 17 15.98 05 16 58.23 05 17 10.02 05 17 02.51 05 17 21.91 05 17 28.64 05 17 29.06 05 17 16.69 05 17 19.40 05 17 00.70 05 17 02.26 05 17 06.13 05 17 22.89 05 16 57.39 05 17 14.58 05 17 09.44 05 17 11.29 05 17 01.21 05 17 10.33 05 17 07.45 05 17 26.87 05 17 14.82 05 17 25.31 05 17 11.59 05 17 15.45 05 17 07.36 05 17 05.00 05 16 57.89 05 17 17.80 05 17 05.88 05 17 14.58 05 17 08.07 05 17 25.68 05 17 02.07 05 16 59.45 05 17 12.37 05 17 16.66 05 17 07.99 05 17 12.90 05 17 14.91 05 17 11.21 05 17 03.03 05 17 23.37 05 17 12.41 05 17 08.41 05 17 11.52 05 17 14.48 05 17 10.52 05 17 20.64 05 17 06.36 05 17 15.30 05 17 18.33 05 17 14.82 05 16 59.51 05 17 10.99 05 17 17.79 05 17 25.53 05 17 13.82 05 17 09.30 05 17 21.77 05 17 12.83 05 17 15.15 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 20 05.7 20 06.1 20 15.5 20 18.6 20 18.6 20 23.7 20 25.5 20 28.7 20 29.9 20 30.1 20 37.2 20 38.8 20 38.6 20 39.9 20 40.1 20 41.5 20 52.6 20 52.9 20 52.9 20 55.0 20 56.3 20 57.8 20 58.9 21 00.4 21 02.1 21 03.3 21 03.5 21 04.8 21 05.0 21 05.2 21 07.0 21 07.5 21 08.0 21 08.6 21 08.9 21 09.5 21 09.5 21 11.2 21 13.9 21 15.7 21 17.0 21 19.9 21 20.1 21 21.2 21 22.4 21 26.6 21 27.5 21 29.3 21 29.6 21 30.8 21 31.1 21 31.5 21 32.3 21 32.9 21 33.0 21 35.2 21 39.1 21 39.6 21 39.9 21 46.8 21 46.7 21 47.7 21 48.3 21 48.2 21 48.4 H (mag) 17.696 ± 0.067 17.414 ± 0.052 17.140 ± 0.068 18.734 ± 0.047 17.635 ± 0.035 18.748 ± 0.051 16.127 ± 0.015 16.961 ± 0.033 15.775 ± 0.021 18.862 ± 0.080 17.603 ± 0.026 17.675 ± 0.022 19.008 ± 0.109 18.578 ± 0.064 18.120 ± 0.030 18.600 ± 0.045 18.697 ± 0.124 17.951 ± 0.029 19.187 ± 0.048 19.419 ± 0.075 17.546 ± 0.032 19.740 ± 0.103 14.695 ± 0.008 17.628 ± 0.036 19.465 ± 0.081 16.220 ± 0.021 18.306 ± 0.028 19.005 ± 0.058 18.724 ± 0.049 19.288 ± 0.065 17.950 ± 0.048 19.088 ± 0.052 18.190 ± 0.025 18.593 ± 0.029 17.322 ± 0.015 17.842 ± 0.045 18.198 ± 0.035 19.369 ± 0.119 15.668 ± 0.008 18.356 ± 0.032 17.103 ± 0.016 18.099 ± 0.021 17.731 ± 0.020 15.388 ± 0.006 18.257 ± 0.040 15.390 ± 0.013 16.859 ± 0.012 14.205 ± 0.006 16.553 ± 0.010 19.221 ± 0.060 19.136 ± 0.056 16.677 ± 0.011 18.935 ± 0.052 18.528 ± 0.029 19.216 ± 0.077 16.148 ± 0.007 15.035 ± 0.013 17.665 ± 0.020 18.696 ± 0.038 16.247 ± 0.025 19.105 ± 0.042 19.116 ± 0.053 19.306 ± 0.091 16.519 ± 0.008 15.979 ± 0.013 Ks (mag) 18.434 ± 0.075 18.193 ± 0.073 18.266 ± 0.058 19.134 ± 0.052 17.840 ± 0.033 19.199 ± 0.045 16.402 ± 0.013 17.446 ± 0.034 16.042 ± 0.017 19.173 ± 0.094 17.967 ± 0.025 18.101 ± 0.029 19.272 ± 0.072 19.035 ± 0.054 18.394 ± 0.027 19.069 ± 0.049 18.947 ± 0.093 18.495 ± 0.028 19.559 ± 0.069 19.938 ± 0.103 17.772 ± 0.021 20.059 ± 0.080 14.893 ± 0.009 17.920 ± 0.035 19.971 ± 0.069 16.442 ± 0.017 18.782 ± 0.030 19.571 ± 0.049 19.095 ± 0.036 19.715 ± 0.072 18.146 ± 0.041 19.453 ± 0.049 18.589 ± 0.029 19.175 ± 0.041 17.695 ± 0.016 18.211 ± 0.031 18.469 ± 0.036 19.712 ± 0.127 15.947 ± 0.007 18.724 ± 0.035 17.419 ± 0.012 18.521 ± 0.025 18.187 ± 0.016 15.788 ± 0.007 18.549 ± 0.034 15.734 ± 0.013 17.293 ± 0.009 14.395 ± 0.008 17.111 ± 0.008 19.560 ± 0.061 19.651 ± 0.074 17.047 ± 0.012 19.528 ± 0.079 19.117 ± 0.040 19.516 ± 0.062 16.559 ± 0.006 15.201 ± 0.011 17.928 ± 0.016 19.202 ± 0.046 16.575 ± 0.015 19.735 ± 0.068 19.553 ± 0.061 19.738 ± 0.078 16.902 ± 0.008 16.523 ± 0.009 H ­ Ks (mag) 0.738 ± 0.101 0.779 ± 0.090 1.126 ± 0.089 0.400 ± 0.070 0.205 ± 0.048 0.451 ± 0.068 0.275 ± 0.020 0.485 ± 0.047 0.267 ± 0.027 0.311 ± 0.123 0.364 ± 0.036 0.426 ± 0.036 0.264 ± 0.131 0.457 ± 0.084 0.274 ± 0.040 0.469 ± 0.067 0.250 ± 0.155 0.544 ± 0.040 0.372 ± 0.084 0.519 ± 0.127 0.226 ± 0.038 0.319 ± 0.130 0.198 ± 0.012 0.292 ± 0.050 0.506 ± 0.106 0.222 ± 0.027 0.476 ± 0.041 0.566 ± 0.076 0.371 ± 0.061 0.427 ± 0.097 0.196 ± 0.063 0.365 ± 0.071 0.399 ± 0.038 0.582 ± 0.050 0.373 ± 0.022 0.369 ± 0.055 0.271 ± 0.050 0.343 ± 0.174 0.279 ± 0.011 0.368 ± 0.047 0.316 ± 0.020 0.422 ± 0.033 0.456 ± 0.026 0.400 ± 0.009 0.292 ± 0.052 0.344 ± 0.018 0.434 ± 0.015 0.190 ± 0.010 0.558 ± 0.013 0.339 ± 0.086 0.515 ± 0.093 0.370 ± 0.016 0.593 ± 0.095 0.589 ± 0.049 0.300 ± 0.099 0.411 ± 0.009 0.166 ± 0.017 0.263 ± 0.026 0.506 ± 0.060 0.328 ± 0.029 0.630 ± 0.080 0.437 ± 0.081 0.432 ± 0.120 0.383 ± 0.011 0.544 ± 0.016


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 12.54 05 17 11.85 05 17 13.90 05 17 15.76 05 17 19.74 05 17 11.56 05 17 14.59 05 17 13.62 05 17 10.06 05 17 09.40 05 17 16.97 05 17 24.55 05 17 08.17 05 17 12.11 05 16 58.47 05 17 15.45 05 17 20.86 05 17 11.37 05 17 16.37 05 17 13.21 05 17 09.23 05 17 12.45 05 17 07.56 05 17 05.48 05 17 03.45 05 17 11.28 05 17 13.29 05 17 14.30 05 17 16.57 05 17 00.27 05 17 15.40 05 17 02.92 05 17 13.94 05 17 13.00 05 17 07.11 05 17 13.12 05 17 07.28 05 17 27.94 05 17 13.93 05 17 12.76 05 17 14.79 05 17 00.83 05 17 06.69 05 17 12.26 05 17 13.49 05 17 13.27 05 17 05.07 05 17 12.55 05 17 09.07 05 17 14.14 05 17 27.62 05 17 12.61 05 17 05.99 05 17 20.14 05 17 13.42 05 17 06.83 05 17 11.32 05 17 14.33 05 17 14.48 05 17 26.57 05 17 17.19 05 17 04.73 05 17 25.47 05 17 12.18 05 17 15.44 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 21 49.8 21 52.5 21 55.2 21 55.5 21 56.6 21 57.1 21 57.7 21 57.9 22 01.8 22 02.2 22 02.6 22 05.4 22 05.3 22 06.3 22 08.2 22 10.0 22 10.7 22 16.1 22 16.6 22 19.2 22 19.7 22 21.4 22 21.4 22 21.4 22 24.3 22 25.3 22 25.5 22 26.2 22 26.2 22 26.5 22 27.2 22 27.5 22 29.0 22 29.0 22 29.1 22 29.9 22 30.0 22 30.3 22 30.3 22 31.1 22 31.3 22 32.1 22 33.0 22 33.3 22 33.4 22 34.2 22 34.9 22 36.2 22 36.1 22 37.0 22 37.3 22 38.4 22 39.9 22 41.0 22 43.2 22 43.4 22 44.5 22 46.9 22 48.3 22 50.8 22 51.4 22 53.5 22 57.0 22 57.6 22 57.8 H (mag) 15.056 ± 0.010 15.949 ± 0.011 18.505 ± 0.035 18.587 ± 0.029 18.184 ± 0.035 14.454 ± 0.005 19.024 ± 0.054 18.334 ± 0.025 19.436 ± 0.069 17.969 ± 0.020 18.095 ± 0.027 14.708 ± 0.016 17.625 ± 0.020 19.418 ± 0.086 18.652 ± 0.075 17.018 ± 0.011 18.142 ± 0.028 15.599 ± 0.006 17.660 ± 0.016 18.809 ± 0.037 17.548 ± 0.019 13.468 ± 0.005 17.492 ± 0.019 16.002 ± 0.009 18.611 ± 0.038 18.064 ± 0.025 18.333 ± 0.030 18.251 ± 0.027 19.855 ± 0.095 18.583 ± 0.053 17.497 ± 0.015 14.693 ± 0.013 17.521 ± 0.021 18.873 ± 0.036 17.971 ± 0.024 17.749 ± 0.016 18.891 ± 0.039 18.398 ± 0.064 18.172 ± 0.024 17.851 ± 0.023 18.727 ± 0.052 18.711 ± 0.071 17.721 ± 0.023 18.941 ± 0.062 17.989 ± 0.019 16.760 ± 0.013 17.262 ± 0.015 14.293 ± 0.006 18.930 ± 0.061 17.666 ± 0.017 18.971 ± 0.107 17.840 ± 0.021 19.187 ± 0.063 18.533 ± 0.038 16.230 ± 0.008 17.867 ± 0.022 15.470 ± 0.006 17.211 ± 0.014 16.979 ± 0.009 19.019 ± 0.110 18.431 ± 0.028 14.107 ± 0.006 19.041 ± 0.105 15.998 ± 0.006 19.005 ± 0.047 Ks (mag) 16.315 ± 0.012 16.635 ± 0.009 19.212 ± 0.048 19.280 ± 0.046 18.555 ± 0.030 15.020 ± 0.004 19.936 ± 0.090 19.077 ± 0.042 19.978 ± 0.074 18.584 ± 0.022 18.431 ± 0.027 14.893 ± 0.015 18.308 ± 0.022 20.127 ± 0.075 18.937 ± 0.061 17.642 ± 0.014 18.463 ± 0.032 15.828 ± 0.006 18.576 ± 0.025 19.497 ± 0.045 17.775 ± 0.012 13.634 ± 0.005 17.907 ± 0.012 16.182 ± 0.007 18.924 ± 0.045 19.522 ± 0.035 19.685 ± 0.069 18.681 ± 0.026 20.278 ± 0.120 18.840 ± 0.064 17.910 ± 0.016 14.897 ± 0.007 17.998 ± 0.017 19.759 ± 0.062 18.541 ± 0.029 18.108 ± 0.015 19.228 ± 0.048 18.762 ± 0.057 18.829 ± 0.035 18.359 ± 0.021 19.250 ± 0.050 19.000 ± 0.052 18.121 ± 0.019 19.373 ± 0.048 18.537 ± 0.026 17.545 ± 0.012 17.634 ± 0.015 14.441 ± 0.005 19.825 ± 0.079 18.095 ± 0.025 19.112 ± 0.090 18.246 ± 0.019 19.519 ± 0.059 18.863 ± 0.034 16.777 ± 0.007 18.399 ± 0.027 15.698 ± 0.004 17.524 ± 0.012 17.296 ± 0.011 19.432 ± 0.127 18.773 ± 0.033 14.307 ± 0.005 19.454 ± 0.157 16.225 ± 0.005 19.304 ± 0.048 H ­ Ks (mag) 1.259 ± 0.016 0.686 ± 0.014 0.707 ± 0.059 0.693 ± 0.054 0.371 ± 0.046 0.566 ± 0.006 0.912 ± 0.105 0.743 ± 0.049 0.542 ± 0.101 0.615 ± 0.030 0.336 ± 0.038 0.185 ± 0.022 0.683 ± 0.030 0.709 ± 0.114 0.285 ± 0.097 0.624 ± 0.018 0.321 ± 0.043 0.229 ± 0.008 0.916 ± 0.030 0.688 ± 0.058 0.227 ± 0.022 0.166 ± 0.007 0.415 ± 0.022 0.180 ± 0.011 0.313 ± 0.059 1.458 ± 0.043 1.352 ± 0.075 0.430 ± 0.037 0.423 ± 0.153 0.257 ± 0.083 0.413 ± 0.022 0.204 ± 0.015 0.477 ± 0.027 0.886 ± 0.072 0.570 ± 0.038 0.359 ± 0.022 0.337 ± 0.062 0.364 ± 0.086 0.657 ± 0.042 0.508 ± 0.031 0.523 ± 0.072 0.289 ± 0.088 0.400 ± 0.030 0.432 ± 0.078 0.548 ± 0.032 0.785 ± 0.018 0.372 ± 0.021 0.148 ± 0.008 0.895 ± 0.100 0.429 ± 0.030 0.141 ± 0.140 0.406 ± 0.028 0.332 ± 0.086 0.330 ± 0.051 0.547 ± 0.011 0.532 ± 0.035 0.228 ± 0.007 0.313 ± 0.018 0.317 ± 0.014 0.413 ± 0.168 0.342 ± 0.043 0.200 ± 0.008 0.413 ± 0.189 0.227 ± 0.008 0.299 ± 0.067

21


22 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 25.30 05 17 17.17 05 17 12.47 05 17 14.56 05 17 29.77 05 17 25.49 05 17 02.18 05 17 04.32 05 17 04.13 05 17 14.28 05 17 04.70 05 17 25.65 05 17 03.71 05 17 22.38 05 16 58.10 05 17 04.93 05 17 25.42 05 17 13.26 05 17 09.31 05 17 09.45 05 16 58.58 05 17 05.03 05 17 08.54 05 17 20.84 05 17 14.21 05 17 14.68 05 17 10.84 05 16 59.84 05 17 18.28 05 17 04.84 05 17 19.16 05 17 13.81 05 16 58.68 05 17 15.29 05 17 17.21 05 17 26.40 05 17 28.45 05 17 20.04 05 17 22.07 05 17 21.79 05 17 12.34 05 17 07.51 05 17 18.40 05 17 08.65 05 17 13.14 05 16 59.00 05 17 15.13 05 16 59.71 05 17 20.30 05 17 14.24 05 17 07.20 05 17 00.08 05 16 59.41 05 17 04.94 05 16 58.65 05 17 15.43 05 17 29.05 05 17 14.48 05 16 58.84 05 17 19.20 05 17 05.73 05 17 00.09 05 17 05.65 05 17 03.58 05 17 07.06

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 23 03.4 23 04.7 23 05.2 23 05.4 23 06.5 23 07.6 23 10.4 23 10.6 23 13.5 23 14.8 23 15.6 23 16.6 23 20.1 23 21.5 23 21.7 23 21.8 23 22.3 23 23.6 23 23.9 23 29.0 23 31.4 23 35.2 23 37.2 23 40.9 23 42.7 23 43.7 23 49.6 23 51.1 23 57.7 24 00.5 24 04.6 24 07.5 24 09.5 24 10.9 24 16.5 24 17.6 24 18.5 24 23.2 24 26.7 24 27.0 20 03.7 20 04.1 20 05.2 20 05.8 20 10.5 20 11.6 20 11.9 20 12.0 20 12.9 20 13.3 20 14.2 20 14.5 20 14.6 20 15.5 20 16.1 20 16.9 20 17.6 20 18.1 20 19.3 20 19.8 20 20.5 20 20.5 20 21.4 20 22.4 20 24.1

H (mag) 18.202 ± 0.051 18.467 ± 0.033 15.480 ± 0.005 18.892 ± 0.044 20.121 ± 0.498 14.941 ± 0.014 18.558 ± 0.056 18.561 ± 0.031 16.655 ± 0.016 17.573 ± 0.017 18.305 ± 0.041 15.578 ± 0.016 13.477 ± 0.023 18.133 ± 0.031 18.025 ± 0.050 18.500 ± 0.034 16.620 ± 0.024 11.338 ± 0.003 19.094 ± 0.051 18.163 ± 0.031 18.194 ± 0.045 18.100 ± 0.029 16.092 ± 0.009 16.898 ± 0.023 11.874 ± 0.005 18.214 ± 0.024 18.289 ± 0.031 18.306 ± 0.057 18.609 ± 0.040 18.337 ± 0.071 18.522 ± 0.051 19.268 ± 0.077 18.409 ± 0.067 17.438 ± 0.063 16.710 ± 0.032 18.994 ± 0.189 19.845 ± 0.344 20.239 ± 0.535 19.721 ± 0.377 19.907 ± 0.458 18.155 ± 0.082 17.910 ± 0.084 17.658 ± 0.056 17.178 ± 0.053 18.122 ± 0.036 15.669 ± 0.027 17.085 ± 0.023 17.722 ± 0.063 18.021 ± 0.032 16.372 ± 0.020 18.915 ± 0.058 18.550 ± 0.067 18.927 ± 0.104 17.772 ± 0.049 18.254 ± 0.056 18.095 ± 0.035 18.130 ± 0.082 14.981 ± 0.012 18.470 ± 0.074 18.841 ± 0.047 17.529 ± 0.045 17.365 ± 0.026 18.944 ± 0.072 19.041 ± 0.074 18.940 ± 0.048

Ks (mag) 18.392 ± 0.044 18.863 ± 0.029 16.119 ± 0.006 19.306 ± 0.047 20.553 ± 0.450 15.142 ± 0.011 18.801 ± 0.050 19.020 ± 0.052 16.898 ± 0.013 17.822 ± 0.015 19.157 ± 0.065 15.842 ± 0.011 13.629 ± 0.010 18.376 ± 0.024 18.085 ± 0.036 18.786 ± 0.035 16.823 ± 0.018 11.549 ± 0.002 19.439 ± 0.054 18.533 ± 0.026 18.475 ± 0.044 18.501 ± 0.027 16.238 ± 0.007 17.109 ± 0.011 11.943 ± 0.003 18.490 ± 0.022 18.488 ± 0.030 18.652 ± 0.047 18.685 ± 0.041 18.520 ± 0.054 18.822 ± 0.034 19.551 ± 0.070 18.623 ± 0.064 18.254 ± 0.050 16.804 ± 0.020 19.232 ± 0.165 20.077 ± 0.375 20.498 ± 0.444 20.185 ± 0.378 20.603 ± 0.513 18.982 ± 0.117 18.652 ± 0.078 18.374 ± 0.080 17.869 ± 0.059 18.582 ± 0.049 15.837 ± 0.025 17.433 ± 0.027 17.934 ± 0.044 18.346 ± 0.034 16.719 ± 0.019 19.398 ± 0.062 18.799 ± 0.057 19.337 ± 0.106 17.667 ± 0.047 18.634 ± 0.050 18.457 ± 0.037 18.705 ± 0.095 15.209 ± 0.017 18.787 ± 0.086 19.371 ± 0.062 17.944 ± 0.037 17.578 ± 0.024 19.354 ± 0.064 19.428 ± 0.082 19.326 ± 0.064

H ­ Ks (mag) 0.190 ± 0.067 0.396 ± 0.044 0.639 ± 0.008 0.414 ± 0.064 0.432 ± 0.671 0.201 ± 0.018 0.243 ± 0.075 0.459 ± 0.061 0.243 ± 0.021 0.249 ± 0.023 0.852 ± 0.077 0.264 ± 0.019 0.152 ± 0.025 0.243 ± 0.039 0.060 ± 0.062 0.286 ± 0.049 0.203 ± 0.030 0.211 ± 0.004 0.345 ± 0.074 0.370 ± 0.040 0.281 ± 0.063 0.401 ± 0.040 0.146 ± 0.011 0.211 ± 0.025 0.069 ± 0.006 0.276 ± 0.033 0.199 ± 0.043 0.346 ± 0.074 0.076 ± 0.057 0.183 ± 0.089 0.300 ± 0.061 0.283 ± 0.104 0.214 ± 0.093 0.816 ± 0.080 0.094 ± 0.038 0.238 ± 0.251 0.232 ± 0.509 0.259 ± 0.695 0.464 ± 0.534 0.696 ± 0.688 0.827 ± 0.143 0.742 ± 0.115 0.716 ± 0.098 0.691 ± 0.079 0.460 ± 0.061 0.168 ± 0.037 0.348 ± 0.035 0.212 ± 0.077 0.325 ± 0.047 0.347 ± 0.028 0.483 ± 0.085 0.249 ± 0.088 0.410 ± 0.148 -0.105 ± 0.068 0.380 ± 0.075 0.362 ± 0.051 0.575 ± 0.125 0.228 ± 0.021 0.317 ± 0.113 0.530 ± 0.078 0.415 ± 0.058 0.213 ± 0.035 0.410 ± 0.096 0.387 ± 0.110 0.386 ± 0.080


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 16 58.99 05 17 10.67 05 17 06.87 05 17 18.53 05 17 21.74 05 17 18.17 05 17 05.54 05 17 00.32 05 17 00.71 05 17 02.10 05 16 58.27 05 17 16.57 05 17 15.37 05 17 02.28 05 17 27.14 05 17 13.62 05 17 11.23 05 16 57.38 05 17 19.31 05 17 10.02 05 17 22.92 05 17 29.69 05 17 28.07 05 17 14.45 05 17 09.60 05 17 19.83 05 17 23.24 05 16 57.59 05 17 21.15 05 17 09.99 05 17 21.90 05 17 26.72 05 17 28.59 05 16 58.13 05 17 28.28 05 17 12.97 05 17 09.92 05 17 16.37 05 16 58.19 05 17 15.63 05 17 07.84 05 17 15.74 05 16 59.12 05 17 10.49 05 17 25.11 05 17 00.40 05 17 16.06 05 17 09.65 05 17 01.67 05 17 04.54 05 17 21.16 05 16 59.35 05 17 10.65 05 17 02.96 05 17 08.58 05 17 08.08 05 17 13.32 05 17 03.94 05 17 12.90 05 17 10.76 05 17 13.26 05 17 19.12 05 17 13.93 05 17 11.33 05 17 05.93 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 20 24.9 20 26.4 20 26.8 20 28.5 20 29.2 20 29.6 20 29.8 20 29.7 20 30.2 20 30.6 20 31.6 20 31.9 20 32.7 20 32.6 20 33.2 20 33.8 20 33.8 20 33.8 20 36.2 20 36.2 20 36.9 20 37.0 20 37.0 20 38.2 20 38.8 20 39.0 20 40.1 20 40.2 20 41.1 20 42.2 20 42.4 20 42.9 20 44.3 20 46.1 20 46.6 20 47.0 20 47.0 20 47.4 20 48.0 20 49.5 20 49.5 20 50.0 20 49.9 20 50.1 20 51.5 20 51.7 20 52.3 20 52.2 20 52.2 20 52.5 20 53.6 20 53.3 20 54.4 20 54.4 20 54.6 20 55.3 20 56.0 20 55.9 20 56.4 20 56.4 20 57.6 20 59.1 20 59.9 20 59.9 21 00.4 H (mag) 17.611 ± 0.030 17.900 ± 0.028 17.962 ± 0.023 18.591 ± 0.039 17.984 ± 0.040 18.141 ± 0.038 17.885 ± 0.035 16.095 ± 0.013 19.612 ± 0.180 16.627 ± 0.019 19.337 ± 0.101 18.138 ± 0.034 18.442 ± 0.037 16.720 ± 0.017 19.152 ± 0.130 14.285 ± 0.012 19.230 ± 0.058 18.040 ± 0.086 16.610 ± 0.017 19.702 ± 0.080 17.769 ± 0.046 18.692 ± 0.104 16.402 ± 0.024 18.960 ± 0.048 19.694 ± 0.091 19.409 ± 0.085 17.655 ± 0.046 17.017 ± 0.034 18.422 ± 0.037 18.428 ± 0.035 18.168 ± 0.030 18.873 ± 0.104 18.059 ± 0.049 14.664 ± 0.017 16.027 ± 0.020 18.047 ± 0.020 18.378 ± 0.027 18.736 ± 0.039 18.885 ± 0.089 19.016 ± 0.047 12.087 ± 0.009 17.429 ± 0.014 15.745 ± 0.014 18.189 ± 0.048 17.290 ± 0.028 17.064 ± 0.021 14.886 ± 0.015 19.051 ± 0.042 16.345 ± 0.018 17.371 ± 0.028 18.040 ± 0.030 18.227 ± 0.041 17.275 ± 0.015 18.633 ± 0.049 18.983 ± 0.045 18.909 ± 0.047 19.141 ± 0.060 18.001 ± 0.037 17.743 ± 0.018 19.208 ± 0.053 18.276 ± 0.028 18.409 ± 0.035 19.341 ± 0.069 19.329 ± 0.085 19.190 ± 0.067 Ks (mag) 17.970 ± 0.026 18.255 ± 0.034 18.357 ± 0.026 18.915 ± 0.050 18.330 ± 0.037 18.471 ± 0.033 18.154 ± 0.031 16.271 ± 0.011 19.773 ± 0.113 16.879 ± 0.016 19.460 ± 0.081 18.531 ± 0.036 18.872 ± 0.035 16.919 ± 0.016 19.458 ± 0.122 14.490 ± 0.014 19.744 ± 0.072 18.261 ± 0.071 16.996 ± 0.016 20.062 ± 0.098 18.213 ± 0.042 18.744 ± 0.085 16.648 ± 0.018 19.435 ± 0.047 20.027 ± 0.088 19.736 ± 0.075 18.008 ± 0.044 17.382 ± 0.027 18.786 ± 0.043 18.779 ± 0.038 18.568 ± 0.040 19.103 ± 0.079 18.512 ± 0.053 14.848 ± 0.016 16.263 ± 0.015 18.356 ± 0.023 18.816 ± 0.028 19.054 ± 0.043 19.512 ± 0.072 19.499 ± 0.071 12.195 ± 0.010 17.694 ± 0.016 15.892 ± 0.014 19.105 ± 0.045 17.658 ± 0.024 17.331 ± 0.024 15.072 ± 0.014 19.584 ± 0.056 16.594 ± 0.014 17.648 ± 0.021 18.456 ± 0.023 18.435 ± 0.046 17.526 ± 0.015 19.138 ± 0.059 19.429 ± 0.059 19.244 ± 0.051 19.664 ± 0.057 18.361 ± 0.030 18.157 ± 0.017 19.627 ± 0.059 18.674 ± 0.035 18.798 ± 0.033 19.781 ± 0.067 19.878 ± 0.069 19.698 ± 0.060 H ­ Ks (mag) 0.359 ± 0.040 0.355 ± 0.044 0.395 ± 0.035 0.324 ± 0.063 0.346 ± 0.054 0.330 ± 0.050 0.269 ± 0.047 0.176 ± 0.017 0.161 ± 0.213 0.252 ± 0.025 0.123 ± 0.129 0.393 ± 0.050 0.430 ± 0.051 0.199 ± 0.023 0.306 ± 0.178 0.205 ± 0.018 0.514 ± 0.092 0.221 ± 0.112 0.386 ± 0.023 0.360 ± 0.127 0.444 ± 0.062 0.052 ± 0.134 0.246 ± 0.030 0.475 ± 0.067 0.333 ± 0.127 0.327 ± 0.113 0.353 ± 0.064 0.365 ± 0.043 0.364 ± 0.057 0.351 ± 0.052 0.400 ± 0.050 0.230 ± 0.131 0.453 ± 0.072 0.184 ± 0.023 0.236 ± 0.025 0.309 ± 0.030 0.438 ± 0.039 0.318 ± 0.058 0.627 ± 0.114 0.483 ± 0.085 0.108 ± 0.013 0.265 ± 0.021 0.147 ± 0.020 0.916 ± 0.066 0.368 ± 0.037 0.267 ± 0.032 0.186 ± 0.021 0.533 ± 0.070 0.249 ± 0.023 0.277 ± 0.035 0.416 ± 0.038 0.208 ± 0.062 0.251 ± 0.021 0.505 ± 0.077 0.446 ± 0.074 0.335 ± 0.069 0.523 ± 0.083 0.360 ± 0.048 0.414 ± 0.025 0.419 ± 0.079 0.398 ± 0.045 0.389 ± 0.048 0.440 ± 0.096 0.549 ± 0.109 0.508 ± 0.090

23


24 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 11.49 05 17 22.68 05 16 58.04 05 17 22.39 05 17 05.88 05 17 06.69 05 16 59.91 05 17 06.59 05 17 08.20 05 17 15.18 05 17 14.20 05 17 08.24 05 17 12.61 05 17 17.78 05 17 08.45 05 17 11.87 05 17 05.69 05 17 03.72 05 17 13.99 05 17 11.64 05 17 12.97 05 17 11.56 05 17 19.63 05 17 12.89 05 17 13.39 05 17 14.90 05 17 00.59 05 17 04.24 05 17 13.92 05 17 11.72 05 17 10.41 05 17 14.08 05 17 14.88 05 17 16.62 05 17 00.45 05 17 07.21 05 17 24.82 05 17 15.93 05 17 14.38 05 16 57.88 05 17 11.20 05 17 03.25 05 17 14.49 05 17 14.52 05 16 59.57 05 17 02.98 05 17 01.83 05 17 04.59 05 17 14.60 05 17 15.57 05 16 59.32 05 17 22.10 05 17 09.67 05 17 12.64 05 17 25.51 05 17 22.52 05 17 12.68 05 17 20.15 05 17 09.90 05 17 16.63 05 17 01.60 05 17 14.27 05 17 09.85 05 17 13.75 05 17 15.29

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 21 00.6 21 01.1 21 01.3 21 01.6 21 01.5 21 02.0 21 02.1 21 02.5 21 02.8 21 03.0 21 03.2 21 03.8 21 04.0 21 04.1 21 04.3 21 04.4 21 04.4 21 04.4 21 04.8 21 04.9 21 05.1 21 06.0 21 06.9 21 06.8 21 07.6 21 07.9 21 08.2 21 08.3 21 08.4 21 08.8 21 09.8 21 10.1 21 10.4 21 10.5 21 10.3 21 10.7 21 11.1 21 11.2 21 11.4 21 11.6 21 12.0 21 12.0 21 12.3 21 13.0 21 12.7 21 12.9 21 13.5 21 13.7 21 14.0 21 14.0 21 14.0 21 14.5 21 14.9 21 15.1 21 15.4 21 16.5 21 16.9 21 17.0 21 17.0 21 17.9 21 18.0 21 18.4 21 18.3 21 18.4 21 18.8

H (mag) 18.412 ± 0.028 16.106 ± 0.017 14.299 ± 0.014 19.022 ± 0.064 17.992 ± 0.023 18.653 ± 0.034 17.878 ± 0.039 15.910 ± 0.009 19.307 ± 0.069 16.659 ± 0.010 18.837 ± 0.034 18.259 ± 0.030 19.359 ± 0.055 18.402 ± 0.036 18.794 ± 0.039 18.669 ± 0.038 13.578 ± 0.010 17.388 ± 0.027 19.576 ± 0.077 17.321 ± 0.020 18.118 ± 0.016 19.796 ± 0.111 19.025 ± 0.055 18.609 ± 0.027 17.230 ± 0.012 18.885 ± 0.050 15.842 ± 0.014 16.786 ± 0.021 16.971 ± 0.011 16.037 ± 0.009 16.530 ± 0.013 13.262 ± 0.007 18.122 ± 0.020 16.173 ± 0.041 16.818 ± 0.019 18.406 ± 0.026 18.623 ± 0.075 15.285 ± 0.007 16.730 ± 0.011 17.327 ± 0.032 19.345 ± 0.055 17.751 ± 0.031 16.482 ± 0.009 18.396 ± 0.031 17.603 ± 0.028 18.172 ± 0.040 17.145 ± 0.023 16.051 ± 0.014 17.865 ± 0.021 19.187 ± 0.058 15.926 ± 0.015 17.623 ± 0.023 18.633 ± 0.033 18.228 ± 0.027 16.433 ± 0.022 17.176 ± 0.020 19.408 ± 0.093 18.589 ± 0.036 18.284 ± 0.028 17.124 ± 0.012 15.333 ± 0.013 15.470 ± 0.006 17.555 ± 0.016 15.864 ± 0.008 19.337 ± 0.080

Ks (mag) 18.860 ± 0.041 16.378 ± 0.020 14.392 ± 0.012 19.513 ± 0.064 18.238 ± 0.021 19.194 ± 0.040 18.190 ± 0.034 16.161 ± 0.010 19.650 ± 0.074 16.924 ± 0.011 19.153 ± 0.037 18.762 ± 0.032 19.706 ± 0.055 18.781 ± 0.038 19.229 ± 0.044 19.373 ± 0.040 13.819 ± 0.010 17.677 ± 0.023 19.784 ± 0.064 17.724 ± 0.017 18.610 ± 0.024 20.152 ± 0.079 19.717 ± 0.075 19.216 ± 0.042 17.579 ± 0.015 19.227 ± 0.045 16.021 ± 0.011 17.019 ± 0.013 17.299 ± 0.011 16.335 ± 0.009 16.762 ± 0.011 13.464 ± 0.008 18.497 ± 0.023 16.475 ± 0.027 17.048 ± 0.019 18.759 ± 0.041 18.681 ± 0.048 15.494 ± 0.009 17.311 ± 0.010 17.487 ± 0.027 19.848 ± 0.064 18.093 ± 0.024 16.885 ± 0.010 18.941 ± 0.048 17.904 ± 0.029 18.513 ± 0.038 17.328 ± 0.016 16.354 ± 0.012 18.318 ± 0.022 19.627 ± 0.067 16.245 ± 0.013 18.005 ± 0.024 18.936 ± 0.034 18.661 ± 0.026 16.672 ± 0.015 17.605 ± 0.019 19.798 ± 0.073 18.946 ± 0.038 18.677 ± 0.025 17.416 ± 0.011 15.591 ± 0.012 15.723 ± 0.007 17.988 ± 0.018 16.216 ± 0.006 19.881 ± 0.092

H ­ Ks (mag) 0.448 ± 0.050 0.272 ± 0.026 0.093 ± 0.018 0.491 ± 0.091 0.246 ± 0.031 0.541 ± 0.052 0.312 ± 0.052 0.251 ± 0.013 0.343 ± 0.101 0.265 ± 0.015 0.316 ± 0.050 0.503 ± 0.044 0.347 ± 0.078 0.379 ± 0.052 0.435 ± 0.059 0.704 ± 0.055 0.241 ± 0.014 0.289 ± 0.035 0.208 ± 0.100 0.403 ± 0.026 0.492 ± 0.029 0.356 ± 0.136 0.692 ± 0.093 0.607 ± 0.050 0.349 ± 0.019 0.342 ± 0.067 0.179 ± 0.018 0.233 ± 0.025 0.328 ± 0.016 0.298 ± 0.013 0.232 ± 0.017 0.202 ± 0.011 0.375 ± 0.030 0.302 ± 0.049 0.230 ± 0.027 0.353 ± 0.049 0.058 ± 0.089 0.209 ± 0.011 0.581 ± 0.015 0.160 ± 0.042 0.503 ± 0.084 0.342 ± 0.039 0.403 ± 0.013 0.545 ± 0.057 0.301 ± 0.040 0.341 ± 0.055 0.183 ± 0.028 0.303 ± 0.018 0.453 ± 0.030 0.440 ± 0.089 0.319 ± 0.020 0.382 ± 0.033 0.303 ± 0.047 0.433 ± 0.037 0.239 ± 0.027 0.429 ± 0.028 0.390 ± 0.118 0.357 ± 0.052 0.393 ± 0.038 0.292 ± 0.016 0.258 ± 0.018 0.253 ± 0.009 0.433 ± 0.024 0.352 ± 0.010 0.544 ± 0.122


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 20.56 05 17 12.62 05 17 12.73 05 17 14.81 05 17 19.08 05 17 24.36 05 17 04.63 05 17 04.65 05 17 14.08 05 17 12.35 05 17 14.45 05 17 23.37 05 16 58.00 05 17 06.40 05 17 01.42 05 17 10.33 05 17 13.66 05 17 04.41 05 17 09.13 05 17 13.45 05 17 15.98 05 17 09.55 05 17 17.43 05 17 00.18 05 17 29.24 05 17 01.15 05 17 02.34 05 17 10.86 05 17 28.17 05 17 15.30 05 17 09.73 05 17 14.00 05 17 13.87 05 17 07.68 05 17 18.23 05 17 04.62 05 17 22.14 05 17 17.32 05 17 14.42 05 17 04.92 05 17 19.48 05 17 15.05 05 17 25.21 05 17 10.99 05 17 05.58 05 17 10.04 05 17 14.72 05 17 11.70 05 17 09.67 05 17 09.12 05 17 12.62 05 17 01.37 05 17 08.79 05 17 11.49 05 17 12.14 05 16 59.24 05 17 15.66 05 17 00.20 05 17 23.78 05 17 09.12 05 17 22.23 05 17 10.07 05 17 24.40 05 17 08.68 05 17 09.80 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 21 19.2 21 20.0 21 20.3 21 20.5 21 21.1 21 21.4 21 21.7 21 22.6 21 22.3 21 22.3 21 22.4 21 22.7 21 22.4 21 23.1 21 23.9 21 24.1 21 24.3 21 24.6 21 24.7 21 25.3 21 25.4 21 25.4 21 25.7 21 26.0 21 26.6 21 28.0 21 28.1 21 28.6 21 28.8 21 28.8 21 28.8 21 29.3 21 31.0 21 31.1 21 31.2 21 31.8 21 32.1 21 32.3 21 32.7 21 32.9 21 33.6 21 33.6 21 33.9 21 33.9 21 34.0 21 34.4 21 34.6 21 34.8 21 35.5 21 35.6 21 35.8 21 36.0 21 36.5 21 36.8 21 37.0 21 37.1 21 37.2 21 37.2 21 38.0 21 38.3 21 38.8 21 38.9 21 39.4 21 39.4 21 39.7 H (mag) 18.655 ± 0.039 19.337 ± 0.069 17.659 ± 0.019 19.534 ± 0.062 18.735 ± 0.049 18.299 ± 0.040 19.373 ± 0.062 17.093 ± 0.017 16.628 ± 0.011 17.940 ± 0.019 17.351 ± 0.013 18.537 ± 0.036 17.888 ± 0.043 18.387 ± 0.029 17.179 ± 0.021 18.115 ± 0.022 16.316 ± 0.008 16.694 ± 0.014 18.032 ± 0.021 17.071 ± 0.013 18.937 ± 0.048 18.936 ± 0.040 18.857 ± 0.039 16.004 ± 0.013 18.156 ± 0.054 16.392 ± 0.021 18.713 ± 0.063 15.806 ± 0.008 16.649 ± 0.026 18.797 ± 0.047 18.394 ± 0.031 18.291 ± 0.032 19.176 ± 0.053 16.857 ± 0.012 18.618 ± 0.043 17.105 ± 0.018 18.110 ± 0.023 16.976 ± 0.013 19.257 ± 0.068 14.964 ± 0.008 17.650 ± 0.019 18.388 ± 0.031 17.685 ± 0.042 17.465 ± 0.013 19.139 ± 0.047 19.273 ± 0.053 19.415 ± 0.080 18.301 ± 0.032 18.472 ± 0.022 17.586 ± 0.018 15.612 ± 0.033 18.360 ± 0.050 15.861 ± 0.008 17.581 ± 0.015 19.223 ± 0.062 17.519 ± 0.032 17.555 ± 0.015 18.376 ± 0.054 17.723 ± 0.026 19.413 ± 0.075 15.419 ± 0.007 16.463 ± 0.014 17.158 ± 0.025 18.163 ± 0.032 17.579 ± 0.018 Ks (mag) 19.281 ± 0.058 19.920 ± 0.072 18.130 ± 0.017 19.922 ± 0.072 19.170 ± 0.049 18.503 ± 0.040 19.738 ± 0.091 17.403 ± 0.014 16.918 ± 0.020 18.399 ± 0.024 18.297 ± 0.019 18.972 ± 0.046 18.085 ± 0.036 18.669 ± 0.033 17.490 ± 0.022 18.646 ± 0.027 16.611 ± 0.008 17.007 ± 0.011 18.484 ± 0.022 17.560 ± 0.010 19.416 ± 0.052 19.311 ± 0.045 19.344 ± 0.047 16.215 ± 0.012 18.412 ± 0.052 16.572 ± 0.014 19.237 ± 0.082 16.479 ± 0.006 16.944 ± 0.020 19.235 ± 0.042 18.852 ± 0.028 18.672 ± 0.030 19.461 ± 0.050 17.243 ± 0.011 18.924 ± 0.032 17.374 ± 0.014 18.448 ± 0.032 17.349 ± 0.009 19.695 ± 0.064 15.146 ± 0.008 18.047 ± 0.021 19.070 ± 0.034 17.887 ± 0.031 17.904 ± 0.014 19.517 ± 0.065 19.616 ± 0.057 19.808 ± 0.084 19.042 ± 0.039 18.986 ± 0.027 18.149 ± 0.018 17.117 ± 0.032 18.674 ± 0.048 16.112 ± 0.006 18.061 ± 0.015 19.508 ± 0.044 17.701 ± 0.027 18.038 ± 0.018 18.844 ± 0.060 17.895 ± 0.022 19.736 ± 0.065 15.643 ± 0.010 17.036 ± 0.010 17.357 ± 0.018 18.501 ± 0.025 18.110 ± 0.014 H ­ Ks (mag) 0.626 ± 0.070 0.583 ± 0.100 0.471 ± 0.025 0.388 ± 0.095 0.435 ± 0.069 0.204 ± 0.057 0.365 ± 0.110 0.310 ± 0.022 0.290 ± 0.023 0.459 ± 0.031 0.946 ± 0.023 0.435 ± 0.058 0.197 ± 0.056 0.282 ± 0.044 0.311 ± 0.030 0.531 ± 0.035 0.295 ± 0.011 0.313 ± 0.018 0.452 ± 0.030 0.489 ± 0.016 0.479 ± 0.071 0.375 ± 0.060 0.487 ± 0.061 0.211 ± 0.018 0.256 ± 0.075 0.180 ± 0.025 0.524 ± 0.103 0.673 ± 0.010 0.295 ± 0.033 0.438 ± 0.063 0.458 ± 0.042 0.381 ± 0.044 0.285 ± 0.073 0.386 ± 0.016 0.306 ± 0.054 0.269 ± 0.023 0.338 ± 0.039 0.373 ± 0.016 0.438 ± 0.093 0.182 ± 0.011 0.397 ± 0.028 0.682 ± 0.046 0.202 ± 0.052 0.439 ± 0.019 0.378 ± 0.080 0.343 ± 0.078 0.393 ± 0.116 0.741 ± 0.050 0.514 ± 0.035 0.563 ± 0.025 1.505 ± 0.046 0.314 ± 0.069 0.251 ± 0.010 0.480 ± 0.021 0.285 ± 0.076 0.182 ± 0.042 0.483 ± 0.023 0.468 ± 0.081 0.172 ± 0.034 0.323 ± 0.099 0.224 ± 0.012 0.573 ± 0.017 0.199 ± 0.031 0.338 ± 0.041 0.531 ± 0.023

25


26 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 10.75 05 17 06.66 05 17 09.60 05 17 19.75 05 17 12.74 05 17 22.72 05 17 20.31 05 17 21.03 05 17 17.31 05 17 17.52 05 16 59.61 05 17 11.58 05 17 14.05 05 17 16.99 05 17 12.46 05 17 06.40 05 17 22.66 05 17 11.64 05 17 11.13 05 17 11.12 05 17 11.31 05 17 16.05 05 17 02.43 05 17 11.98 05 17 07.92 05 17 06.37 05 17 18.63 05 17 15.34 05 17 17.98 05 17 14.59 05 17 12.19 05 17 01.99 05 17 26.68 05 17 21.52 05 17 10.84 05 17 13.23 05 17 09.36 05 17 24.77 05 17 17.48 05 17 16.01 05 16 58.62 05 17 05.29 05 17 09.60 05 17 15.19 05 17 15.73 05 17 19.48 05 17 07.27 05 17 11.60 05 17 12.46 05 17 02.02 05 17 11.28 05 17 12.81 05 16 58.48 05 17 10.80 05 17 07.71 05 17 13.90 05 17 09.68 05 17 13.44 05 17 11.07 05 17 15.19 05 17 12.16 05 17 14.41 05 17 14.11 05 17 12.35 05 17 13.35

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 21 40.6 21 40.7 21 40.8 21 40.9 21 41.0 21 41.2 21 42.7 21 42.9 21 42.9 21 43.4 21 43.5 21 43.8 21 44.8 21 45.0 21 45.1 21 45.2 21 45.4 21 45.6 21 45.9 21 46.6 21 46.3 21 47.4 21 47.3 21 47.9 21 47.9 21 48.1 21 48.6 21 48.8 21 49.0 21 49.4 21 49.4 21 49.5 21 49.9 21 49.9 21 49.8 21 49.9 21 50.0 21 50.7 21 50.7 21 50.7 21 50.5 21 50.8 21 51.0 21 51.1 21 51.2 21 51.4 21 51.3 21 51.4 21 51.5 21 51.4 21 51.7 21 51.8 21 51.6 21 52.2 21 52.4 21 52.4 21 52.5 21 52.8 21 53.2 21 53.7 21 53.7 21 53.9 21 54.0 21 54.1 21 54.4

H (mag) 16.486 ± 0.008 18.067 ± 0.029 17.432 ± 0.015 18.234 ± 0.036 19.142 ± 0.053 17.161 ± 0.016 15.931 ± 0.007 17.980 ± 0.030 19.361 ± 0.067 19.195 ± 0.056 17.213 ± 0.023 17.323 ± 0.014 16.822 ± 0.011 14.823 ± 0.006 17.617 ± 0.020 18.560 ± 0.039 18.755 ± 0.050 17.384 ± 0.017 15.589 ± 0.006 16.144 ± 0.007 17.029 ± 0.008 17.459 ± 0.016 18.409 ± 0.046 13.360 ± 0.053 16.809 ± 0.017 19.546 ± 0.084 18.892 ± 0.047 18.416 ± 0.032 15.261 ± 0.011 18.118 ± 0.020 17.581 ± 0.014 17.417 ± 0.032 19.083 ± 0.115 16.951 ± 0.012 16.275 ± 0.009 18.701 ± 0.044 18.255 ± 0.028 17.846 ± 0.043 16.000 ± 0.009 16.182 ± 0.007 18.981 ± 0.082 19.637 ± 0.102 17.905 ± 0.019 19.363 ± 0.064 19.208 ± 0.062 18.100 ± 0.031 18.516 ± 0.059 17.125 ± 0.013 16.793 ± 0.011 16.435 ± 0.018 16.514 ± 0.010 19.469 ± 0.079 18.223 ± 0.043 18.479 ± 0.032 17.508 ± 0.039 19.642 ± 0.097 19.485 ± 0.077 13.651 ± 0.005 18.889 ± 0.043 17.515 ± 0.016 16.249 ± 0.007 17.801 ± 0.018 17.336 ± 0.023 17.429 ± 0.019 14.509 ± 0.006

Ks (mag) 17.293 ± 0.008 18.875 ± 0.042 18.065 ± 0.016 18.724 ± 0.034 19.466 ± 0.059 17.466 ± 0.016 16.192 ± 0.008 18.295 ± 0.028 19.740 ± 0.072 19.737 ± 0.060 17.498 ± 0.022 18.615 ± 0.026 17.425 ± 0.011 15.150 ± 0.007 19.283 ± 0.040 18.945 ± 0.031 19.170 ± 0.046 17.730 ± 0.015 16.497 ± 0.006 16.886 ± 0.008 17.280 ± 0.011 17.882 ± 0.015 18.747 ± 0.047 13.979 ± 0.032 17.005 ± 0.008 20.350 ± 0.109 19.326 ± 0.058 19.037 ± 0.037 15.448 ± 0.013 18.867 ± 0.027 17.775 ± 0.019 17.606 ± 0.024 19.322 ± 0.133 17.277 ± 0.013 16.461 ± 0.011 19.110 ± 0.044 19.003 ± 0.036 18.067 ± 0.030 16.277 ± 0.010 16.815 ± 0.007 19.477 ± 0.082 20.016 ± 0.096 18.387 ± 0.020 19.998 ± 0.086 19.792 ± 0.073 18.440 ± 0.027 19.717 ± 0.071 18.207 ± 0.019 17.856 ± 0.013 16.639 ± 0.011 17.734 ± 0.012 19.668 ± 0.068 18.649 ± 0.041 19.053 ± 0.028 17.730 ± 0.026 19.986 ± 0.066 19.971 ± 0.066 14.092 ± 0.006 19.342 ± 0.046 18.069 ± 0.016 16.564 ± 0.007 18.455 ± 0.025 17.790 ± 0.021 18.919 ± 0.039 14.935 ± 0.005

H ­ Ks (mag) 0.807 ± 0.011 0.808 ± 0.051 0.633 ± 0.022 0.490 ± 0.050 0.324 ± 0.079 0.305 ± 0.023 0.261 ± 0.011 0.315 ± 0.041 0.379 ± 0.098 0.542 ± 0.082 0.285 ± 0.032 1.292 ± 0.030 0.603 ± 0.016 0.327 ± 0.009 1.666 ± 0.045 0.385 ± 0.050 0.415 ± 0.068 0.346 ± 0.023 0.908 ± 0.008 0.742 ± 0.011 0.251 ± 0.014 0.423 ± 0.022 0.338 ± 0.066 0.619 ± 0.062 0.196 ± 0.019 0.804 ± 0.138 0.434 ± 0.075 0.621 ± 0.049 0.187 ± 0.017 0.749 ± 0.034 0.194 ± 0.024 0.189 ± 0.040 0.239 ± 0.176 0.326 ± 0.018 0.186 ± 0.014 0.409 ± 0.062 0.748 ± 0.046 0.221 ± 0.052 0.277 ± 0.013 0.633 ± 0.010 0.496 ± 0.116 0.379 ± 0.140 0.482 ± 0.028 0.635 ± 0.107 0.584 ± 0.096 0.340 ± 0.041 1.201 ± 0.092 1.082 ± 0.023 1.063 ± 0.017 0.204 ± 0.021 1.220 ± 0.016 0.199 ± 0.104 0.426 ± 0.059 0.574 ± 0.043 0.222 ± 0.047 0.344 ± 0.117 0.486 ± 0.101 0.441 ± 0.008 0.453 ± 0.063 0.554 ± 0.023 0.315 ± 0.010 0.654 ± 0.031 0.454 ± 0.031 1.490 ± 0.043 0.426 ± 0.008


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 13.55 05 17 11.80 05 17 17.67 05 17 22.56 05 17 09.90 05 17 12.68 05 17 14.68 05 17 15.88 05 17 14.39 05 17 15.00 05 16 57.77 05 17 14.18 05 17 10.86 05 17 12.99 05 17 09.82 05 17 17.06 05 17 14.28 05 17 16.38 05 17 20.18 05 17 12.45 05 16 59.48 05 17 17.63 05 17 12.90 05 17 12.29 05 17 09.80 05 17 17.73 05 17 14.46 05 17 14.77 05 17 11.58 05 17 13.90 05 17 19.76 05 17 10.74 05 17 03.29 05 17 03.17 05 17 02.82 05 17 13.42 05 17 13.46 05 17 21.34 05 17 10.96 05 17 11.22 05 17 14.91 05 17 09.45 05 17 02.67 05 17 04.19 05 17 22.49 05 17 14.59 05 17 09.03 05 17 10.95 05 17 13.84 05 17 10.63 05 17 17.21 05 17 22.87 05 17 23.84 05 17 15.55 05 17 16.51 05 17 14.92 05 17 10.93 05 17 18.20 05 17 23.46 05 17 17.99 05 17 09.74 05 16 57.60 05 17 23.08 05 17 19.41 05 17 16.60 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 21 54.6 21 55.0 21 55.1 21 55.2 21 55.4 21 55.5 21 56.1 21 56.4 21 56.5 21 57.0 21 57.0 21 57.3 21 57.3 21 57.6 21 57.7 21 58.0 21 58.1 21 58.2 21 58.9 21 59.2 21 59.1 21 59.3 21 59.4 21 59.7 21 59.8 21 59.9 22 00.1 22 00.1 22 00.4 22 00.7 22 00.8 22 00.9 22 01.0 22 01.2 22 01.2 22 01.8 22 02.0 22 02.5 22 02.4 22 02.4 22 03.2 22 03.3 22 03.2 22 03.8 22 04.3 22 04.7 22 04.8 22 04.9 22 05.2 22 05.3 22 05.6 22 05.7 22 05.8 22 05.8 22 06.2 22 06.2 22 06.5 22 07.0 22 07.2 22 07.2 22 07.1 22 07.0 22 07.4 22 07.8 22 07.9 H (mag) 14.548 ± 0.006 14.964 ± 0.005 17.544 ± 0.018 18.974 ± 0.057 15.625 ± 0.006 15.487 ± 0.006 19.555 ± 0.080 16.882 ± 0.010 19.265 ± 0.091 19.480 ± 0.070 15.100 ± 0.018 16.447 ± 0.009 19.520 ± 0.055 18.299 ± 0.025 19.409 ± 0.068 17.990 ± 0.018 17.117 ± 0.027 15.764 ± 0.007 17.673 ± 0.020 16.486 ± 0.010 15.827 ± 0.013 17.900 ± 0.024 17.962 ± 0.019 17.773 ± 0.019 19.396 ± 0.068 18.303 ± 0.025 15.215 ± 0.005 18.153 ± 0.020 17.781 ± 0.019 18.996 ± 0.051 17.551 ± 0.019 18.145 ± 0.024 18.574 ± 0.045 17.821 ± 0.027 14.845 ± 0.014 18.286 ± 0.031 16.320 ± 0.009 17.637 ± 0.021 14.922 ± 0.005 17.693 ± 0.018 16.826 ± 0.012 17.426 ± 0.014 18.318 ± 0.051 18.085 ± 0.029 17.236 ± 0.016 14.605 ± 0.004 17.654 ± 0.019 17.396 ± 0.014 17.162 ± 0.012 18.177 ± 0.024 17.371 ± 0.012 16.971 ± 0.011 18.591 ± 0.051 17.924 ± 0.022 15.543 ± 0.006 18.570 ± 0.036 18.356 ± 0.026 17.138 ± 0.014 18.399 ± 0.032 19.393 ± 0.071 18.471 ± 0.032 14.569 ± 0.022 17.522 ± 0.024 13.137 ± 0.006 18.839 ± 0.038 Ks (mag) 15.053 ± 0.006 15.654 ± 0.004 17.791 ± 0.016 19.337 ± 0.056 15.828 ± 0.004 16.273 ± 0.006 20.218 ± 0.099 17.598 ± 0.011 20.126 ± 0.113 19.836 ± 0.096 15.218 ± 0.010 17.301 ± 0.011 20.002 ± 0.078 18.948 ± 0.033 19.722 ± 0.065 18.327 ± 0.021 17.862 ± 0.019 16.057 ± 0.007 18.003 ± 0.024 16.712 ± 0.007 16.059 ± 0.012 18.464 ± 0.024 18.604 ± 0.022 18.265 ± 0.020 20.097 ± 0.091 18.774 ± 0.030 15.789 ± 0.005 18.997 ± 0.032 18.249 ± 0.018 19.750 ± 0.063 17.931 ± 0.019 18.550 ± 0.025 19.064 ± 0.043 18.186 ± 0.025 15.190 ± 0.009 18.532 ± 0.036 17.081 ± 0.008 18.016 ± 0.024 15.353 ± 0.004 18.053 ± 0.016 17.245 ± 0.008 18.279 ± 0.022 18.644 ± 0.036 18.421 ± 0.030 17.532 ± 0.016 15.179 ± 0.005 18.053 ± 0.015 17.777 ± 0.015 17.413 ± 0.010 18.498 ± 0.021 17.837 ± 0.015 17.245 ± 0.015 18.861 ± 0.052 19.533 ± 0.053 15.777 ± 0.006 19.277 ± 0.043 18.826 ± 0.032 17.603 ± 0.012 18.805 ± 0.040 19.523 ± 0.057 19.103 ± 0.040 14.746 ± 0.012 17.818 ± 0.020 13.287 ± 0.008 19.312 ± 0.050 H ­ Ks (mag) 0.505 ± 0.008 0.690 ± 0.006 0.247 ± 0.024 0.363 ± 0.080 0.203 ± 0.007 0.786 ± 0.008 0.663 ± 0.127 0.716 ± 0.015 0.861 ± 0.145 0.356 ± 0.119 0.118 ± 0.021 0.854 ± 0.014 0.482 ± 0.095 0.649 ± 0.041 0.313 ± 0.094 0.337 ± 0.028 0.745 ± 0.033 0.293 ± 0.010 0.330 ± 0.031 0.226 ± 0.012 0.232 ± 0.018 0.564 ± 0.034 0.642 ± 0.029 0.492 ± 0.028 0.701 ± 0.114 0.471 ± 0.039 0.574 ± 0.007 0.844 ± 0.038 0.468 ± 0.026 0.754 ± 0.081 0.380 ± 0.027 0.405 ± 0.035 0.490 ± 0.062 0.365 ± 0.037 0.345 ± 0.017 0.246 ± 0.048 0.761 ± 0.012 0.379 ± 0.032 0.431 ± 0.006 0.360 ± 0.024 0.419 ± 0.014 0.853 ± 0.026 0.326 ± 0.062 0.336 ± 0.042 0.296 ± 0.023 0.574 ± 0.006 0.399 ± 0.024 0.381 ± 0.021 0.251 ± 0.016 0.321 ± 0.032 0.466 ± 0.019 0.274 ± 0.019 0.270 ± 0.073 1.609 ± 0.057 0.234 ± 0.008 0.707 ± 0.056 0.470 ± 0.041 0.465 ± 0.018 0.406 ± 0.051 0.130 ± 0.091 0.632 ± 0.051 0.177 ± 0.025 0.296 ± 0.031 0.150 ± 0.010 0.473 ± 0.063

27


28 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 00.77 05 17 15.04 05 17 10.86 05 17 14.90 05 17 13.28 05 17 14.15 05 17 12.67 05 17 12.53 05 17 16.97 05 17 16.00 05 17 16.36 05 17 27.81 05 17 14.25 05 17 12.33 05 17 06.56 05 17 10.51 05 17 23.09 05 16 59.56 05 16 58.87 05 17 14.13 05 17 11.25 05 17 16.11 05 17 09.14 05 17 10.34 05 17 16.15 05 17 07.72 05 17 12.62 05 16 59.59 05 17 15.84 05 17 00.04 05 17 23.49 05 17 03.00 05 17 24.83 05 17 14.00 05 17 14.62 05 17 15.99 05 17 06.01 05 17 22.58 05 17 15.26 05 17 07.90 05 17 29.15 05 17 17.03 05 17 13.08 05 17 22.78 05 17 09.71 05 17 14.08 05 17 17.27 05 17 28.26 05 17 10.14 05 17 09.57 05 17 05.36 05 17 15.53 05 17 07.61 05 17 21.64 05 17 14.90 05 17 02.14 05 17 11.99 05 17 11.61 05 17 29.43 05 17 13.31 05 17 26.06 05 17 11.13 05 17 14.52 05 17 22.65 05 17 13.17

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 22 08.1 22 08.8 22 09.5 22 09.5 22 09.6 22 09.8 22 10.6 22 10.7 22 10.9 22 11.3 22 12.2 22 12.6 22 12.8 22 12.9 22 12.9 22 13.4 22 13.7 22 13.5 22 13.5 22 13.8 22 13.9 22 14.0 22 14.3 22 14.4 22 15.5 22 15.6 22 15.8 22 15.8 22 16.3 22 16.1 22 16.8 22 16.7 22 17.1 22 17.6 22 17.1 22 17.1 22 17.4 22 17.7 22 17.9 22 17.8 22 18.3 22 18.3 22 18.3 22 18.8 22 18.7 22 18.8 22 19.1 22 19.2 22 19.3 22 19.5 22 19.5 22 19.7 22 19.6 22 19.8 22 19.9 22 19.7 22 19.9 22 20.1 22 20.3 22 20.4 22 21.2 22 21.3 22 21.4 22 21.7 22 21.7

H (mag) 18.048 ± 0.046 18.128 ± 0.027 18.390 ± 0.026 19.067 ± 0.047 19.310 ± 0.072 18.441 ± 0.029 18.946 ± 0.040 18.530 ± 0.028 18.820 ± 0.044 15.831 ± 0.006 16.663 ± 0.008 17.687 ± 0.046 17.828 ± 0.022 17.770 ± 0.017 18.909 ± 0.051 18.543 ± 0.031 19.194 ± 0.078 15.565 ± 0.013 18.854 ± 0.065 17.148 ± 0.050 18.641 ± 0.035 15.086 ± 0.005 13.144 ± 0.004 19.272 ± 0.069 18.087 ± 0.027 15.245 ± 0.007 18.720 ± 0.046 19.330 ± 0.124 15.401 ± 0.005 16.867 ± 0.017 18.333 ± 0.039 19.227 ± 0.084 18.978 ± 0.072 15.303 ± 0.018 18.018 ± 0.021 17.421 ± 0.014 19.153 ± 0.060 16.818 ± 0.014 17.912 ± 0.031 17.215 ± 0.016 17.662 ± 0.080 18.922 ± 0.049 16.901 ± 0.012 19.579 ± 0.108 16.623 ± 0.009 17.095 ± 0.013 16.856 ± 0.009 15.142 ± 0.015 17.735 ± 0.020 19.365 ± 0.074 18.787 ± 0.038 16.093 ± 0.008 14.306 ± 0.007 17.222 ± 0.016 16.733 ± 0.010 16.747 ± 0.019 17.878 ± 0.022 16.930 ± 0.013 17.520 ± 0.030 18.488 ± 0.041 18.296 ± 0.070 18.733 ± 0.037 18.725 ± 0.053 15.800 ± 0.010 16.601 ± 0.010

Ks (mag) 18.363 ± 0.033 18.976 ± 0.036 19.080 ± 0.042 19.708 ± 0.044 19.753 ± 0.055 18.976 ± 0.032 19.469 ± 0.045 19.150 ± 0.042 19.219 ± 0.040 16.255 ± 0.006 17.476 ± 0.011 18.143 ± 0.037 18.969 ± 0.036 18.261 ± 0.022 19.324 ± 0.060 18.957 ± 0.032 19.642 ± 0.078 15.723 ± 0.010 19.405 ± 0.096 17.925 ± 0.031 19.076 ± 0.037 15.272 ± 0.006 13.241 ± 0.003 19.606 ± 0.061 19.068 ± 0.043 15.443 ± 0.005 19.365 ± 0.045 19.536 ± 0.132 16.065 ± 0.007 17.088 ± 0.017 18.733 ± 0.031 19.778 ± 0.106 19.070 ± 0.066 17.549 ± 0.021 18.553 ± 0.023 18.184 ± 0.018 19.494 ± 0.058 17.074 ± 0.013 18.468 ± 0.022 17.625 ± 0.015 18.333 ± 0.069 19.454 ± 0.047 17.817 ± 0.075 19.777 ± 0.084 16.981 ± 0.008 18.689 ± 0.032 17.102 ± 0.010 15.445 ± 0.015 17.968 ± 0.016 19.864 ± 0.075 19.382 ± 0.059 16.430 ± 0.007 14.475 ± 0.005 17.565 ± 0.014 17.549 ± 0.009 16.989 ± 0.015 18.403 ± 0.023 17.363 ± 0.011 17.709 ± 0.027 19.176 ± 0.039 18.661 ± 0.062 19.311 ± 0.047 19.816 ± 0.090 16.112 ± 0.009 17.614 ± 0.010

H ­ Ks (mag) 0.315 ± 0.057 0.848 ± 0.045 0.690 ± 0.049 0.641 ± 0.064 0.443 ± 0.091 0.535 ± 0.043 0.523 ± 0.060 0.620 ± 0.050 0.399 ± 0.059 0.424 ± 0.008 0.813 ± 0.014 0.456 ± 0.059 1.141 ± 0.042 0.491 ± 0.028 0.415 ± 0.079 0.414 ± 0.045 0.448 ± 0.110 0.158 ± 0.016 0.551 ± 0.116 0.777 ± 0.059 0.435 ± 0.051 0.186 ± 0.008 0.097 ± 0.005 0.334 ± 0.092 0.981 ± 0.051 0.198 ± 0.009 0.645 ± 0.064 0.206 ± 0.181 0.664 ± 0.009 0.221 ± 0.024 0.400 ± 0.050 0.551 ± 0.135 0.092 ± 0.098 2.246 ± 0.028 0.535 ± 0.031 0.763 ± 0.023 0.341 ± 0.083 0.256 ± 0.019 0.556 ± 0.038 0.410 ± 0.022 0.671 ± 0.106 0.532 ± 0.068 0.916 ± 0.076 0.198 ± 0.137 0.358 ± 0.012 1.594 ± 0.035 0.246 ± 0.013 0.303 ± 0.021 0.233 ± 0.026 0.499 ± 0.105 0.595 ± 0.070 0.337 ± 0.011 0.169 ± 0.009 0.343 ± 0.021 0.816 ± 0.013 0.242 ± 0.024 0.525 ± 0.032 0.433 ± 0.017 0.189 ± 0.040 0.688 ± 0.057 0.365 ± 0.094 0.578 ± 0.060 1.091 ± 0.104 0.312 ± 0.013 1.013 ± 0.014


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 21.87 05 17 06.60 05 17 22.44 05 17 13.24 05 17 13.29 05 17 06.74 05 17 11.50 05 17 28.23 05 16 59.71 05 17 13.48 05 17 11.10 05 17 12.96 05 17 13.64 05 17 10.73 05 17 01.52 05 16 59.53 05 17 16.74 05 17 22.56 05 17 11.97 05 17 14.85 05 17 13.94 05 17 13.84 05 17 27.34 05 17 14.96 05 17 21.76 05 17 14.08 05 17 13.67 05 17 12.53 05 17 09.30 05 16 59.57 05 17 13.40 05 17 10.21 05 17 12.44 05 17 15.05 05 17 12.73 05 17 05.16 05 17 21.61 05 17 15.57 05 17 08.52 05 17 13.30 05 17 13.73 05 17 14.40 05 17 10.62 05 17 14.05 05 17 14.32 05 17 17.64 05 17 08.97 05 17 12.62 05 17 13.80 05 17 13.62 05 17 16.71 05 17 14.74 05 17 11.28 05 17 12.84 05 17 07.55 05 16 58.80 05 17 09.70 05 17 04.80 05 17 13.79 05 17 21.74 05 17 19.45 05 17 12.89 05 16 58.57 05 17 02.85 05 17 14.22 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 22 21.7 22 22.0 22 22.1 22 22.9 22 23.4 22 22.8 22 22.9 22 23.1 22 23.2 22 23.8 22 24.0 22 24.1 22 24.2 22 24.3 22 24.2 22 24.2 22 24.5 22 24.6 22 24.9 22 26.1 22 26.2 22 26.4 22 26.6 22 26.7 22 27.3 22 27.3 22 27.4 22 27.5 22 27.8 22 27.8 22 28.0 22 28.3 22 28.9 22 29.3 22 29.3 22 29.3 22 29.6 22 29.6 22 29.8 22 29.9 22 30.0 22 30.1 22 30.1 22 30.3 22 30.9 22 31.1 22 31.4 22 31.5 22 31.6 22 31.8 22 32.1 22 32.3 22 32.6 22 32.9 22 33.6 22 33.6 22 33.8 22 33.8 22 34.3 22 34.4 22 34.7 22 35.0 22 35.0 22 35.2 22 35.6 H (mag) 19.410 ± 0.093 16.047 ± 0.008 19.749 ± 0.128 16.161 ± 0.007 17.805 ± 0.018 19.204 ± 0.065 17.113 ± 0.010 18.059 ± 0.055 16.543 ± 0.019 15.439 ± 0.045 19.298 ± 0.075 17.648 ± 0.016 17.060 ± 0.019 15.922 ± 0.006 17.610 ± 0.034 14.716 ± 0.012 18.836 ± 0.031 18.684 ± 0.053 17.737 ± 0.019 18.322 ± 0.028 17.939 ± 0.020 18.324 ± 0.030 14.314 ± 0.015 17.853 ± 0.022 16.239 ± 0.012 18.278 ± 0.033 17.200 ± 0.015 18.629 ± 0.041 19.151 ± 0.070 17.564 ± 0.028 17.864 ± 0.063 18.628 ± 0.034 18.085 ± 0.027 18.682 ± 0.056 18.509 ± 0.025 15.085 ± 0.010 18.831 ± 0.059 13.088 ± 0.005 18.752 ± 0.041 17.957 ± 0.019 15.769 ± 0.007 18.140 ± 0.024 18.273 ± 0.027 17.219 ± 0.018 19.235 ± 0.056 18.299 ± 0.031 19.149 ± 0.064 18.587 ± 0.031 16.662 ± 0.011 15.435 ± 0.007 19.182 ± 0.060 18.804 ± 0.047 19.583 ± 0.084 18.114 ± 0.025 19.007 ± 0.059 14.840 ± 0.011 18.214 ± 0.028 16.325 ± 0.008 17.549 ± 0.017 19.080 ± 0.056 14.955 ± 0.006 16.119 ± 0.008 18.239 ± 0.056 17.437 ± 0.023 16.868 ± 0.010 Ks (mag) 19.825 ± 0.083 16.334 ± 0.007 19.864 ± 0.096 17.573 ± 0.011 19.096 ± 0.037 19.894 ± 0.087 17.509 ± 0.012 18.294 ± 0.051 16.683 ± 0.012 16.190 ± 0.029 19.789 ± 0.061 19.710 ± 0.059 17.624 ± 0.015 16.128 ± 0.005 17.862 ± 0.027 14.818 ± 0.007 19.275 ± 0.051 19.051 ± 0.043 18.173 ± 0.019 18.943 ± 0.031 18.674 ± 0.032 18.949 ± 0.036 14.497 ± 0.011 18.499 ± 0.021 16.448 ± 0.010 19.100 ± 0.043 17.799 ± 0.013 19.068 ± 0.035 19.852 ± 0.073 17.784 ± 0.022 19.136 ± 0.043 19.368 ± 0.043 18.764 ± 0.022 19.195 ± 0.047 18.868 ± 0.032 15.257 ± 0.009 19.129 ± 0.049 13.253 ± 0.005 19.291 ± 0.057 18.369 ± 0.021 16.064 ± 0.006 18.951 ± 0.042 18.595 ± 0.026 17.484 ± 0.013 19.667 ± 0.063 18.537 ± 0.023 19.616 ± 0.069 18.919 ± 0.027 17.250 ± 0.010 15.672 ± 0.006 19.778 ± 0.058 19.269 ± 0.041 20.242 ± 0.104 18.668 ± 0.029 19.534 ± 0.051 15.016 ± 0.007 18.504 ± 0.019 16.653 ± 0.009 17.999 ± 0.014 19.514 ± 0.062 15.159 ± 0.007 16.343 ± 0.005 18.559 ± 0.046 17.822 ± 0.019 17.486 ± 0.010 H ­ Ks (mag) 0.415 ± 0.125 0.287 ± 0.011 0.115 ± 0.160 1.412 ± 0.013 1.291 ± 0.041 0.690 ± 0.109 0.396 ± 0.016 0.235 ± 0.075 0.140 ± 0.022 0.751 ± 0.054 0.491 ± 0.097 2.062 ± 0.061 0.564 ± 0.024 0.206 ± 0.008 0.252 ± 0.043 0.102 ± 0.014 0.439 ± 0.060 0.367 ± 0.068 0.436 ± 0.027 0.621 ± 0.042 0.735 ± 0.038 0.625 ± 0.047 0.183 ± 0.019 0.646 ± 0.030 0.209 ± 0.016 0.822 ± 0.054 0.599 ± 0.020 0.439 ± 0.054 0.701 ± 0.101 0.220 ± 0.036 1.272 ± 0.076 0.740 ± 0.055 0.679 ± 0.035 0.513 ± 0.073 0.359 ± 0.041 0.172 ± 0.013 0.298 ± 0.077 0.165 ± 0.007 0.539 ± 0.070 0.412 ± 0.028 0.295 ± 0.009 0.811 ± 0.048 0.322 ± 0.037 0.265 ± 0.022 0.432 ± 0.084 0.238 ± 0.039 0.467 ± 0.094 0.332 ± 0.041 0.588 ± 0.015 0.237 ± 0.009 0.596 ± 0.083 0.465 ± 0.062 0.659 ± 0.134 0.554 ± 0.038 0.527 ± 0.078 0.176 ± 0.013 0.290 ± 0.034 0.328 ± 0.012 0.450 ± 0.022 0.434 ± 0.084 0.204 ± 0.009 0.224 ± 0.009 0.320 ± 0.072 0.385 ± 0.030 0.618 ± 0.014

29


30 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 28.28 05 17 13.66 05 17 08.20 05 17 12.31 05 17 11.91 05 17 12.87 05 17 16.44 05 17 08.98 05 17 02.08 05 17 19.81 05 17 25.00 05 17 10.13 05 16 59.96 05 17 13.83 05 17 15.75 05 17 06.91 05 17 22.21 05 17 08.45 05 17 11.61 05 17 08.20 05 17 02.97 05 17 12.60 05 16 58.32 05 17 12.92 05 17 09.38 05 17 29.12 05 16 58.04 05 17 09.90 05 17 09.04 05 17 29.78 05 17 18.43 05 17 16.57 05 17 11.68 05 17 13.34 05 17 09.93 05 17 15.84 05 17 12.56 05 17 07.18 05 17 13.57 05 17 08.72 05 17 03.06 05 17 13.69 05 16 58.14 05 17 16.63 05 17 13.60 05 17 24.85 05 17 22.65 05 17 10.78 05 17 17.69 05 17 16.91 05 17 10.16 05 17 17.58 05 17 14.35 05 17 09.35 05 17 12.00 05 17 13.33 05 17 03.61 05 17 01.60 05 17 21.60 05 17 02.10 05 17 12.84 05 17 03.12 05 17 17.00 05 17 22.73 05 17 18.51

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 22 36.2 22 36.4 22 36.5 22 36.8 22 36.9 22 37.8 22 38.0 22 38.6 22 38.6 22 38.8 22 38.9 22 39.2 22 39.0 22 39.3 22 39.3 22 39.2 22 39.7 22 39.7 22 39.8 22 40.2 22 40.3 22 40.5 22 40.4 22 40.9 22 41.8 22 42.9 22 43.0 22 43.9 22 43.9 22 44.4 22 44.8 22 44.8 22 45.4 22 45.8 22 46.0 22 46.5 22 46.8 22 47.1 22 47.6 22 47.7 22 47.8 22 48.2 22 48.4 22 48.6 22 48.7 22 49.1 22 49.1 22 49.7 22 50.0 22 51.2 22 51.4 22 51.6 22 51.9 22 52.2 22 52.4 22 52.4 22 52.5 22 52.7 22 53.1 22 53.2 22 53.4 22 54.0 22 54.4 22 54.5 22 55.0

H (mag) 18.913 ± 0.106 15.705 ± 0.006 17.023 ± 0.016 16.519 ± 0.007 19.161 ± 0.058 17.502 ± 0.016 19.772 ± 0.108 16.266 ± 0.008 18.148 ± 0.042 17.671 ± 0.021 18.248 ± 0.052 18.995 ± 0.053 16.214 ± 0.015 17.427 ± 0.017 17.493 ± 0.012 15.994 ± 0.008 19.607 ± 0.081 18.883 ± 0.051 16.833 ± 0.011 17.944 ± 0.017 18.342 ± 0.048 18.409 ± 0.028 14.998 ± 0.010 18.008 ± 0.020 17.161 ± 0.011 17.293 ± 0.036 18.292 ± 0.068 19.457 ± 0.077 16.663 ± 0.010 13.304 ± 0.040 19.084 ± 0.048 19.266 ± 0.056 18.439 ± 0.030 19.150 ± 0.045 17.102 ± 0.010 17.777 ± 0.018 16.504 ± 0.012 18.094 ± 0.026 17.664 ± 0.022 19.057 ± 0.054 18.621 ± 0.051 18.321 ± 0.031 16.740 ± 0.025 17.585 ± 0.017 18.046 ± 0.024 18.504 ± 0.067 19.510 ± 0.093 17.253 ± 0.014 19.237 ± 0.070 17.200 ± 0.012 18.608 ± 0.031 19.435 ± 0.072 17.898 ± 0.021 15.950 ± 0.009 19.104 ± 0.079 18.425 ± 0.031 16.961 ± 0.015 14.512 ± 0.011 17.704 ± 0.025 15.753 ± 0.012 19.160 ± 0.057 19.002 ± 0.076 17.986 ± 0.025 17.025 ± 0.019 18.191 ± 0.050

Ks (mag) 19.102 ± 0.085 15.919 ± 0.005 18.402 ± 0.028 16.848 ± 0.008 19.551 ± 0.059 18.069 ± 0.018 20.238 ± 0.091 16.906 ± 0.007 18.569 ± 0.045 17.961 ± 0.021 18.481 ± 0.050 19.272 ± 0.042 16.495 ± 0.012 18.028 ± 0.021 17.818 ± 0.018 16.195 ± 0.007 19.783 ± 0.085 19.445 ± 0.061 17.102 ± 0.009 18.366 ± 0.021 18.736 ± 0.040 18.829 ± 0.026 15.113 ± 0.008 18.372 ± 0.019 17.396 ± 0.011 17.685 ± 0.032 18.491 ± 0.052 19.968 ± 0.081 17.176 ± 0.009 13.505 ± 0.028 19.411 ± 0.048 19.544 ± 0.050 18.800 ± 0.035 19.664 ± 0.059 17.481 ± 0.010 18.144 ± 0.016 16.796 ± 0.005 18.547 ± 0.024 18.151 ± 0.017 19.393 ± 0.053 19.027 ± 0.055 18.748 ± 0.028 16.912 ± 0.021 17.873 ± 0.015 18.338 ± 0.017 18.734 ± 0.052 19.745 ± 0.080 17.551 ± 0.012 19.569 ± 0.062 17.503 ± 0.010 19.024 ± 0.032 19.640 ± 0.069 18.271 ± 0.017 16.279 ± 0.004 19.945 ± 0.098 19.146 ± 0.032 17.265 ± 0.012 14.738 ± 0.006 17.980 ± 0.020 15.909 ± 0.009 19.543 ± 0.051 19.221 ± 0.053 18.297 ± 0.017 17.355 ± 0.012 18.276 ± 0.059

H ­ Ks (mag) 0.189 ± 0.136 0.214 ± 0.008 1.379 ± 0.032 0.329 ± 0.011 0.390 ± 0.083 0.567 ± 0.024 0.466 ± 0.141 0.640 ± 0.011 0.421 ± 0.062 0.290 ± 0.030 0.233 ± 0.072 0.277 ± 0.068 0.281 ± 0.019 0.601 ± 0.027 0.325 ± 0.022 0.201 ± 0.011 0.176 ± 0.117 0.562 ± 0.080 0.269 ± 0.014 0.422 ± 0.027 0.394 ± 0.062 0.420 ± 0.038 0.115 ± 0.013 0.364 ± 0.028 0.235 ± 0.016 0.392 ± 0.048 0.199 ± 0.086 0.511 ± 0.112 0.513 ± 0.013 0.201 ± 0.049 0.327 ± 0.068 0.278 ± 0.075 0.361 ± 0.046 0.514 ± 0.074 0.379 ± 0.014 0.367 ± 0.024 0.292 ± 0.013 0.453 ± 0.035 0.487 ± 0.028 0.336 ± 0.076 0.406 ± 0.075 0.427 ± 0.042 0.172 ± 0.033 0.288 ± 0.023 0.292 ± 0.029 0.230 ± 0.085 0.235 ± 0.123 0.298 ± 0.018 0.332 ± 0.094 0.303 ± 0.016 0.416 ± 0.045 0.205 ± 0.100 0.373 ± 0.027 0.329 ± 0.010 0.841 ± 0.126 0.721 ± 0.045 0.304 ± 0.019 0.226 ± 0.013 0.276 ± 0.032 0.156 ± 0.015 0.383 ± 0.076 0.219 ± 0.093 0.311 ± 0.030 0.330 ± 0.022 0.085 ± 0.077


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 16.75 05 17 13.45 05 16 59.74 05 17 00.74 05 17 11.29 05 17 29.37 05 17 02.09 05 17 01.56 05 17 12.49 05 17 13.90 05 17 26.13 05 16 58.02 05 17 17.17 05 17 15.53 05 17 29.76 05 17 06.62 05 17 19.26 05 17 16.69 05 17 04.33 05 17 00.76 05 17 04.77 05 17 14.02 05 17 21.63 05 17 00.79 05 16 59.74 05 17 14.42 05 17 17.51 05 17 11.84 05 17 20.35 05 17 05.83 05 17 21.15 05 17 23.90 05 16 59.32 05 17 27.57 05 17 01.18 05 17 11.51 05 16 59.55 05 17 13.47 05 17 06.63 05 17 15.83 05 17 12.69 05 17 10.20 05 17 02.33 05 17 25.61 05 17 22.77 05 17 10.41 05 17 29.24 05 17 07.40 05 17 00.56 05 17 09.51 05 17 09.96 05 17 29.38 05 17 09.19 05 17 08.10 05 17 07.21 05 17 19.07 05 16 58.98 05 17 12.30 05 17 05.53 05 17 21.71 05 16 57.48 05 16 58.53 05 17 21.32 05 17 14.49 05 17 11.14 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 22 55.1 22 55.7 22 56.2 22 56.6 22 56.8 22 57.7 22 57.7 22 58.3 22 58.8 22 59.5 23 00.2 23 00.6 23 01.5 23 01.5 23 01.6 23 01.7 23 02.6 23 02.7 23 02.9 23 03.4 23 03.9 23 04.4 23 04.7 23 04.8 23 05.0 23 05.4 23 05.6 23 06.0 23 06.7 23 06.9 23 07.7 23 07.8 23 08.1 23 08.8 23 09.1 23 09.3 23 09.2 23 09.6 23 09.5 23 09.7 23 09.7 23 10.0 23 10.3 23 10.9 23 10.9 23 11.3 23 11.6 23 12.0 23 12.4 23 12.6 23 13.4 23 14.1 23 14.3 23 14.6 23 14.9 23 15.5 23 16.2 23 17.2 23 17.2 23 17.4 23 18.6 23 18.9 23 19.7 23 21.6 23 21.9 H (mag) 17.139 ± 0.013 17.864 ± 0.019 17.888 ± 0.032 15.359 ± 0.011 17.162 ± 0.012 18.533 ± 0.073 16.699 ± 0.019 17.075 ± 0.021 16.730 ± 0.009 18.697 ± 0.038 16.856 ± 0.030 18.618 ± 0.084 18.000 ± 0.020 18.827 ± 0.037 17.890 ± 0.077 17.614 ± 0.020 16.677 ± 0.012 19.165 ± 0.061 16.740 ± 0.012 17.953 ± 0.035 11.104 ± 0.006 16.511 ± 0.009 17.772 ± 0.021 14.344 ± 0.010 18.538 ± 0.061 17.900 ± 0.018 16.139 ± 0.014 19.521 ± 0.079 16.973 ± 0.011 19.225 ± 0.053 18.024 ± 0.031 18.083 ± 0.038 17.716 ± 0.032 17.919 ± 0.045 17.162 ± 0.023 15.942 ± 0.007 17.912 ± 0.042 15.647 ± 0.006 19.502 ± 0.088 14.866 ± 0.004 17.563 ± 0.013 18.731 ± 0.032 18.042 ± 0.045 17.956 ± 0.050 17.713 ± 0.036 14.549 ± 0.005 14.079 ± 0.025 17.809 ± 0.023 18.197 ± 0.055 17.224 ± 0.013 18.326 ± 0.029 17.003 ± 0.028 19.081 ± 0.053 17.941 ± 0.021 16.595 ± 0.010 16.406 ± 0.013 17.185 ± 0.021 19.701 ± 0.095 16.643 ± 0.010 18.957 ± 0.067 18.708 ± 0.134 14.785 ± 0.015 18.921 ± 0.071 16.025 ± 0.005 15.075 ± 0.005 Ks (mag) 17.384 ± 0.012 18.221 ± 0.018 18.069 ± 0.030 15.535 ± 0.008 17.619 ± 0.013 18.608 ± 0.055 17.476 ± 0.019 17.432 ± 0.017 17.033 ± 0.009 19.166 ± 0.041 17.096 ± 0.020 19.447 ± 0.098 18.283 ± 0.023 19.246 ± 0.045 17.940 ± 0.042 17.986 ± 0.019 16.928 ± 0.011 19.525 ± 0.063 16.939 ± 0.006 18.669 ± 0.055 11.334 ± 0.003 16.706 ± 0.006 18.086 ± 0.020 14.452 ± 0.007 18.894 ± 0.056 18.144 ± 0.020 16.400 ± 0.011 19.986 ± 0.066 17.286 ± 0.012 19.414 ± 0.058 18.189 ± 0.021 18.317 ± 0.028 17.963 ± 0.028 18.135 ± 0.038 17.404 ± 0.018 16.179 ± 0.005 18.186 ± 0.031 15.810 ± 0.005 19.855 ± 0.084 15.063 ± 0.005 17.959 ± 0.013 19.105 ± 0.041 18.361 ± 0.036 18.298 ± 0.047 17.948 ± 0.021 14.672 ± 0.003 14.260 ± 0.016 18.014 ± 0.014 18.485 ± 0.047 17.452 ± 0.010 18.647 ± 0.020 17.117 ± 0.023 19.363 ± 0.050 18.211 ± 0.020 16.758 ± 0.009 16.709 ± 0.008 17.409 ± 0.017 19.979 ± 0.091 16.842 ± 0.009 20.082 ± 0.099 18.944 ± 0.114 14.958 ± 0.006 19.911 ± 0.112 16.352 ± 0.004 15.229 ± 0.004 H ­ Ks (mag) 0.245 ± 0.018 0.357 ± 0.026 0.181 ± 0.044 0.176 ± 0.014 0.457 ± 0.018 0.075 ± 0.091 0.777 ± 0.027 0.357 ± 0.027 0.303 ± 0.013 0.469 ± 0.056 0.240 ± 0.036 0.829 ± 0.129 0.283 ± 0.030 0.419 ± 0.058 0.050 ± 0.088 0.372 ± 0.028 0.251 ± 0.016 0.360 ± 0.088 0.199 ± 0.013 0.716 ± 0.065 0.230 ± 0.007 0.195 ± 0.011 0.314 ± 0.029 0.108 ± 0.012 0.356 ± 0.083 0.244 ± 0.027 0.261 ± 0.018 0.465 ± 0.103 0.313 ± 0.016 0.189 ± 0.079 0.165 ± 0.037 0.234 ± 0.047 0.247 ± 0.043 0.216 ± 0.059 0.242 ± 0.029 0.237 ± 0.009 0.274 ± 0.052 0.163 ± 0.008 0.353 ± 0.122 0.197 ± 0.006 0.396 ± 0.018 0.374 ± 0.052 0.319 ± 0.058 0.342 ± 0.069 0.235 ± 0.042 0.123 ± 0.006 0.181 ± 0.030 0.205 ± 0.027 0.288 ± 0.072 0.228 ± 0.016 0.321 ± 0.035 0.114 ± 0.036 0.282 ± 0.073 0.270 ± 0.029 0.163 ± 0.013 0.303 ± 0.015 0.224 ± 0.027 0.278 ± 0.132 0.199 ± 0.013 1.125 ± 0.120 0.236 ± 0.176 0.173 ± 0.016 0.990 ± 0.133 0.327 ± 0.006 0.154 ± 0.006

31


32 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 20.35 05 17 22.28 05 17 23.25 05 17 03.87 05 17 17.53 05 16 58.40 05 17 27.46 05 17 08.82 05 17 15.79 05 17 23.21 05 17 14.93 05 17 02.59 05 17 10.33 05 17 22.20 05 17 28.07 05 17 13.57 05 16 57.60 05 17 08.04 05 17 27.09 05 17 20.15 05 17 20.01 05 17 12.87 05 17 11.71 05 17 07.11 05 17 14.97 05 17 21.74 05 17 27.97 05 17 19.52 05 17 11.38 05 17 21.41 05 17 00.30 05 17 20.96 05 17 07.94 05 17 14.48 05 17 12.76 05 17 02.69 05 17 24.25 05 17 06.27 05 17 14.20 05 16 58.44 05 17 10.09 05 17 04.67 05 17 00.11 05 17 05.87 05 17 13.70 05 17 24.96 05 17 01.45 05 17 01.78 05 17 05.10 05 17 11.65 05 17 12.57 05 16 58.82 05 17 13.32 05 17 01.46 05 17 10.66 05 17 10.08 05 17 09.23 05 16 59.08 05 17 26.74 05 17 20.44 05 17 04.04 05 16 57.95 05 17 06.71 05 17 24.01 05 17 00.93

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 23 22.7 23 22.8 23 22.9 23 22.8 23 23.3 23 23.2 23 24.0 23 24.0 23 24.3 23 24.5 23 25.5 23 25.6 23 26.1 23 27.0 23 28.0 23 28.0 23 28.2 23 28.5 23 28.7 23 28.9 23 29.2 23 29.9 23 31.1 23 32.5 23 32.8 23 33.0 23 33.4 23 33.7 23 33.9 23 34.1 23 34.6 23 34.9 23 35.1 23 35.2 23 35.8 23 36.5 23 36.9 23 36.7 23 36.9 23 36.7 23 38.3 23 38.9 23 39.0 23 39.3 23 40.0 23 40.2 23 40.4 23 40.5 23 40.9 23 42.7 23 42.9 23 43.1 23 43.9 23 44.4 23 46.0 23 46.5 23 47.1 23 47.4 23 48.4 23 48.5 23 48.9 23 48.8 23 49.5 23 50.1 23 50.6

H (mag) 18.596 ± 0.038 16.909 ± 0.025 18.975 ± 0.069 19.419 ± 0.075 17.964 ± 0.027 18.493 ± 0.067 16.921 ± 0.030 18.218 ± 0.024 17.028 ± 0.015 18.828 ± 0.053 18.656 ± 0.037 18.201 ± 0.045 19.139 ± 0.053 16.669 ± 0.024 18.846 ± 0.118 17.731 ± 0.014 17.593 ± 0.053 16.675 ± 0.013 16.140 ± 0.022 19.481 ± 0.096 19.037 ± 0.072 15.766 ± 0.005 19.545 ± 0.102 18.816 ± 0.043 17.582 ± 0.017 18.626 ± 0.051 15.866 ± 0.025 18.171 ± 0.032 15.877 ± 0.009 19.209 ± 0.067 17.682 ± 0.030 18.571 ± 0.049 19.663 ± 0.096 19.690 ± 0.094 18.856 ± 0.042 17.997 ± 0.048 18.521 ± 0.077 18.415 ± 0.036 18.462 ± 0.032 17.934 ± 0.038 18.067 ± 0.027 16.502 ± 0.036 16.200 ± 0.020 16.777 ± 0.017 18.059 ± 0.025 15.836 ± 0.018 18.706 ± 0.070 13.913 ± 0.012 18.198 ± 0.033 18.042 ± 0.020 18.898 ± 0.044 16.473 ± 0.030 17.315 ± 0.013 17.593 ± 0.035 18.841 ± 0.045 18.389 ± 0.035 18.673 ± 0.046 17.749 ± 0.042 16.975 ± 0.027 16.880 ± 0.024 16.847 ± 0.064 17.241 ± 0.033 17.263 ± 0.017 17.588 ± 0.033 19.117 ± 0.087

Ks (mag) 18.959 ± 0.043 17.109 ± 0.013 18.506 ± 0.106 20.116 ± 0.121 18.176 ± 0.023 18.731 ± 0.053 17.068 ± 0.021 18.580 ± 0.027 17.253 ± 0.008 19.081 ± 0.049 18.989 ± 0.036 18.434 ± 0.037 19.372 ± 0.052 16.948 ± 0.013 19.258 ± 0.083 17.925 ± 0.015 17.802 ± 0.049 16.932 ± 0.009 16.395 ± 0.014 19.825 ± 0.093 19.392 ± 0.059 15.922 ± 0.004 20.047 ± 0.089 19.214 ± 0.038 17.831 ± 0.015 18.926 ± 0.043 16.106 ± 0.013 18.411 ± 0.033 16.054 ± 0.004 19.643 ± 0.078 17.974 ± 0.032 18.853 ± 0.041 19.997 ± 0.120 20.050 ± 0.076 19.157 ± 0.034 18.130 ± 0.028 18.539 ± 0.054 18.798 ± 0.035 18.690 ± 0.025 18.214 ± 0.031 18.278 ± 0.018 16.709 ± 0.027 16.348 ± 0.010 17.063 ± 0.011 18.283 ± 0.016 16.084 ± 0.012 19.258 ± 0.080 14.048 ± 0.007 18.484 ± 0.030 18.351 ± 0.021 19.229 ± 0.051 16.728 ± 0.018 17.543 ± 0.012 17.748 ± 0.030 19.126 ± 0.043 18.717 ± 0.031 19.036 ± 0.033 17.991 ± 0.029 17.203 ± 0.022 17.242 ± 0.012 17.066 ± 0.045 17.349 ± 0.025 17.470 ± 0.014 17.402 ± 0.032 19.540 ± 0.090

H ­ Ks (mag) 0.363 ± 0.057 0.200 ± 0.028 -0.469 ± 0.126 0.697 ± 0.142 0.212 ± 0.035 0.238 ± 0.085 0.147 ± 0.037 0.362 ± 0.036 0.225 ± 0.017 0.253 ± 0.072 0.333 ± 0.052 0.233 ± 0.058 0.233 ± 0.074 0.279 ± 0.027 0.412 ± 0.144 0.194 ± 0.021 0.209 ± 0.072 0.257 ± 0.016 0.255 ± 0.026 0.344 ± 0.134 0.355 ± 0.093 0.156 ± 0.006 0.502 ± 0.135 0.398 ± 0.057 0.249 ± 0.023 0.300 ± 0.067 0.240 ± 0.028 0.240 ± 0.046 0.177 ± 0.010 0.434 ± 0.103 0.292 ± 0.044 0.282 ± 0.064 0.334 ± 0.154 0.360 ± 0.121 0.301 ± 0.054 0.133 ± 0.056 0.018 ± 0.094 0.383 ± 0.050 0.228 ± 0.041 0.280 ± 0.049 0.211 ± 0.032 0.207 ± 0.045 0.148 ± 0.022 0.286 ± 0.020 0.224 ± 0.030 0.248 ± 0.022 0.552 ± 0.106 0.135 ± 0.014 0.286 ± 0.045 0.309 ± 0.029 0.331 ± 0.067 0.255 ± 0.035 0.228 ± 0.018 0.155 ± 0.046 0.285 ± 0.062 0.328 ± 0.047 0.363 ± 0.057 0.242 ± 0.051 0.228 ± 0.035 0.362 ± 0.027 0.219 ± 0.078 0.108 ± 0.041 0.207 ± 0.022 -0.186 ± 0.046 0.423 ± 0.125


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 05.43 05 17 01.47 05 16 59.26 05 17 01.91 05 17 05.95 05 17 10.92 05 17 19.64 05 17 08.76 05 17 08.66 05 17 27.66 05 17 26.31 05 17 13.19 05 17 16.10 05 17 17.49 05 17 01.66 05 17 13.95 05 17 06.72 05 17 01.79 05 16 59.86 05 16 58.12 05 16 58.72 05 17 21.92 05 17 12.72 05 17 26.09 05 17 07.40 05 17 26.91 05 17 12.47 05 17 08.27 05 17 00.45 05 17 13.94 05 17 12.28 05 17 06.33 05 17 12.41 05 17 14.26 05 17 13.19 05 17 12.85 05 16 59.39 05 17 05.27 05 17 08.97 05 17 24.98 05 17 04.67 05 17 28.64 05 17 23.32 05 16 58.04 05 16 57.60 05 17 08.88 05 17 05.41 05 17 03.78 05 17 10.82 05 17 18.48 05 17 20.24 05 17 15.28 05 17 03.64 05 17 13.33 05 17 01.45 05 17 18.14 05 17 10.57 05 17 18.76 05 17 00.77 05 17 20.66 05 17 08.00 05 17 27.33 05 17 19.12 05 17 08.63 05 17 21.45 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 23 51.0 23 51.2 23 51.3 23 51.7 23 51.9 23 52.1 23 52.4 23 52.8 23 53.8 23 54.8 23 55.4 23 55.3 23 55.7 23 56.4 23 57.0 23 58.7 23 59.4 24 00.5 24 00.9 24 01.1 24 01.2 24 02.4 24 02.9 24 03.1 24 05.1 24 05.8 24 06.0 24 07.4 24 08.7 24 08.9 24 10.3 24 10.4 24 10.8 24 11.5 24 12.1 24 13.3 24 13.5 24 14.5 24 15.2 24 15.5 24 16.3 24 16.8 24 17.7 24 18.6 24 19.3 24 20.6 24 21.5 24 22.1 24 22.4 20 03.8 20 04.2 20 07.4 20 08.1 20 08.3 20 09.0 20 10.7 20 11.2 20 12.1 20 11.9 20 14.4 20 18.0 20 19.2 20 19.5 20 19.5 20 20.3 H (mag) 15.041 ± 0.041 16.404 ± 0.017 15.157 ± 0.035 18.178 ± 0.046 19.145 ± 0.064 18.247 ± 0.029 18.819 ± 0.073 18.489 ± 0.034 18.691 ± 0.052 17.643 ± 0.061 16.050 ± 0.027 16.163 ± 0.009 19.178 ± 0.064 19.575 ± 0.095 17.435 ± 0.029 19.316 ± 0.066 15.404 ± 0.030 18.560 ± 0.067 17.945 ± 0.054 16.954 ± 0.035 17.884 ± 0.051 19.092 ± 0.080 17.765 ± 0.018 18.773 ± 0.116 16.118 ± 0.027 18.195 ± 0.067 15.610 ± 0.017 18.218 ± 0.038 17.285 ± 0.034 18.136 ± 0.033 18.219 ± 0.046 17.126 ± 0.060 19.225 ± 0.093 19.451 ± 0.115 17.419 ± 0.023 19.455 ± 0.102 17.249 ± 0.047 18.051 ± 0.043 18.091 ± 0.049 18.123 ± 0.072 18.869 ± 0.099 17.683 ± 0.058 18.610 ± 0.095 16.357 ± 0.030 17.807 ± 0.050 16.221 ± 0.021 16.429 ± 0.056 17.673 ± 0.058 17.347 ± 0.035 17.091 ± 0.048 18.329 ± 0.093 17.144 ± 0.038 18.088 ± 0.077 18.154 ± 0.046 19.906 ± 0.351 18.970 ± 0.079 17.583 ± 0.035 18.450 ± 0.045 14.229 ± 0.023 16.388 ± 0.022 14.911 ± 0.019 16.032 ± 0.016 18.766 ± 0.039 17.107 ± 0.018 17.639 ± 0.037 Ks (mag) 15.199 ± 0.028 16.575 ± 0.012 15.281 ± 0.021 18.342 ± 0.031 19.451 ± 0.058 18.584 ± 0.023 19.127 ± 0.051 18.778 ± 0.047 18.886 ± 0.039 17.761 ± 0.036 16.289 ± 0.016 16.423 ± 0.008 19.327 ± 0.055 19.918 ± 0.087 17.695 ± 0.025 19.806 ± 0.077 15.586 ± 0.021 18.880 ± 0.062 18.226 ± 0.035 17.169 ± 0.032 18.173 ± 0.038 19.413 ± 0.070 18.013 ± 0.018 19.627 ± 0.130 16.275 ± 0.015 18.428 ± 0.055 15.755 ± 0.013 18.448 ± 0.031 17.380 ± 0.025 18.471 ± 0.027 18.552 ± 0.032 17.314 ± 0.041 19.390 ± 0.071 19.783 ± 0.111 17.578 ± 0.017 19.717 ± 0.099 17.342 ± 0.036 17.819 ± 0.042 18.244 ± 0.030 18.274 ± 0.068 19.094 ± 0.102 18.047 ± 0.067 18.785 ± 0.080 16.573 ± 0.025 18.097 ± 0.063 16.322 ± 0.010 16.592 ± 0.027 18.246 ± 0.067 17.588 ± 0.040 18.276 ± 0.074 19.368 ± 0.111 17.541 ± 0.038 18.651 ± 0.071 18.706 ± 0.053 20.424 ± 0.402 19.756 ± 0.111 17.918 ± 0.028 18.854 ± 0.052 14.371 ± 0.017 16.789 ± 0.027 15.127 ± 0.013 16.439 ± 0.027 19.100 ± 0.041 17.683 ± 0.019 17.943 ± 0.028 H ­ Ks (mag) 0.158 ± 0.050 0.171 ± 0.021 0.124 ± 0.041 0.164 ± 0.055 0.306 ± 0.086 0.337 ± 0.037 0.308 ± 0.089 0.289 ± 0.058 0.195 ± 0.065 0.118 ± 0.071 0.239 ± 0.031 0.260 ± 0.012 0.149 ± 0.084 0.343 ± 0.129 0.260 ± 0.038 0.490 ± 0.101 0.182 ± 0.037 0.320 ± 0.091 0.281 ± 0.064 0.215 ± 0.047 0.289 ± 0.064 0.321 ± 0.106 0.248 ± 0.025 0.854 ± 0.174 0.157 ± 0.031 0.233 ± 0.087 0.145 ± 0.021 0.230 ± 0.049 0.095 ± 0.042 0.335 ± 0.043 0.333 ± 0.056 0.188 ± 0.073 0.165 ± 0.117 0.332 ± 0.160 0.159 ± 0.029 0.262 ± 0.142 0.093 ± 0.059 -0.232 ± 0.060 0.153 ± 0.057 0.151 ± 0.099 0.225 ± 0.142 0.364 ± 0.089 0.175 ± 0.124 0.216 ± 0.039 0.290 ± 0.080 0.101 ± 0.023 0.163 ± 0.062 0.573 ± 0.089 0.241 ± 0.053 1.185 ± 0.088 1.039 ± 0.145 0.397 ± 0.054 0.563 ± 0.105 0.552 ± 0.070 0.518 ± 0.534 0.786 ± 0.136 0.335 ± 0.045 0.404 ± 0.069 0.142 ± 0.029 0.401 ± 0.035 0.216 ± 0.023 0.407 ± 0.031 0.334 ± 0.057 0.576 ± 0.026 0.304 ± 0.046

33


34 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 16.82 05 17 11.83 05 17 15.19 05 17 09.61 05 17 29.02 05 17 25.30 05 17 11.86 05 17 25.29 05 17 27.65 05 17 19.76 05 17 19.72 05 17 16.35 05 17 10.70 05 17 04.64 05 17 26.76 05 17 07.59 05 17 06.72 05 17 08.94 05 17 22.06 05 17 27.06 05 17 23.81 05 17 20.80 05 17 03.66 05 17 28.32 05 17 00.26 05 17 13.06 05 17 12.31 05 17 04.38 05 17 10.73 05 17 06.65 05 17 00.14 05 17 21.85 05 16 57.82 05 17 18.79 05 17 11.57 05 17 10.73 05 17 18.79 05 17 10.45 05 17 27.83 05 17 20.18 05 17 10.60 05 17 10.15 05 17 01.70 05 17 11.16 05 17 18.92 05 17 21.79 05 16 57.62 05 17 23.64 05 17 03.69 05 17 25.64 05 17 03.44 05 17 26.37 05 17 13.36 05 17 28.46 05 17 13.81 05 17 14.56 05 17 29.97 05 17 12.17 05 17 25.40 05 17 14.12 05 17 13.30 05 17 08.02 05 17 08.47 05 16 59.74 05 17 25.88

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 20 21.0 20 21.3 20 22.0 20 23.8 20 26.0 20 27.4 20 27.8 20 29.5 20 31.3 20 31.5 20 32.9 20 33.4 20 36.1 20 38.5 20 41.7 20 41.8 20 41.9 20 42.2 20 43.7 20 44.1 20 44.9 20 46.2 20 46.4 20 48.2 20 49.4 20 50.5 20 52.2 20 52.3 20 53.2 20 53.1 20 54.4 20 54.7 20 56.8 20 58.0 20 58.5 20 58.8 21 02.5 21 02.4 21 04.6 21 07.3 21 07.6 21 08.2 21 09.3 21 10.4 21 10.5 21 11.6 21 13.1 21 14.5 21 14.4 21 16.2 21 15.9 21 16.8 21 18.1 21 20.5 21 20.4 21 20.5 21 22.1 21 23.0 21 23.8 21 24.3 21 24.5 21 27.4 21 30.2 21 31.6 21 32.0

H (mag) 18.651 ± 0.048 16.062 ± 0.023 14.149 ± 0.023 17.480 ± 0.029 16.909 ± 0.035 16.854 ± 0.027 16.649 ± 0.016 15.685 ± 0.022 18.790 ± 0.109 18.880 ± 0.049 17.683 ± 0.030 19.445 ± 0.072 15.245 ± 0.022 12.639 ± 0.038 18.883 ± 0.103 13.003 ± 0.011 14.715 ± 0.013 16.696 ± 0.022 18.969 ± 0.056 15.611 ± 0.022 17.750 ± 0.043 18.069 ± 0.036 17.466 ± 0.045 14.230 ± 0.020 17.638 ± 0.034 17.714 ± 0.030 16.920 ± 0.013 18.955 ± 0.064 18.595 ± 0.046 18.274 ± 0.047 17.855 ± 0.034 17.360 ± 0.024 15.253 ± 0.015 18.621 ± 0.047 18.197 ± 0.022 19.950 ± 0.131 18.445 ± 0.032 17.293 ± 0.013 16.773 ± 0.025 18.908 ± 0.057 19.221 ± 0.065 15.612 ± 0.010 16.298 ± 0.028 18.787 ± 0.039 17.430 ± 0.026 19.201 ± 0.066 16.596 ± 0.028 12.762 ± 0.024 15.875 ± 0.018 17.265 ± 0.034 18.274 ± 0.031 17.269 ± 0.030 17.689 ± 0.021 18.289 ± 0.052 19.882 ± 0.094 19.354 ± 0.045 17.525 ± 0.053 18.724 ± 0.033 16.612 ± 0.025 19.053 ± 0.054 18.022 ± 0.020 18.459 ± 0.032 16.805 ± 0.013 18.774 ± 0.067 17.321 ± 0.036

Ks (mag) 19.009 ± 0.046 16.289 ± 0.019 14.385 ± 0.024 17.851 ± 0.020 17.169 ± 0.027 17.117 ± 0.019 16.892 ± 0.021 15.929 ± 0.016 19.232 ± 0.084 19.308 ± 0.054 18.044 ± 0.028 19.914 ± 0.066 15.501 ± 0.019 12.791 ± 0.024 19.079 ± 0.088 13.134 ± 0.011 14.905 ± 0.011 16.946 ± 0.017 19.425 ± 0.063 15.898 ± 0.014 18.025 ± 0.034 18.409 ± 0.034 17.773 ± 0.036 14.423 ± 0.014 17.946 ± 0.029 18.125 ± 0.025 17.186 ± 0.014 19.303 ± 0.059 19.027 ± 0.049 19.321 ± 0.061 18.156 ± 0.031 17.675 ± 0.018 15.370 ± 0.012 18.991 ± 0.039 18.696 ± 0.023 20.282 ± 0.121 18.842 ± 0.036 17.637 ± 0.015 17.016 ± 0.022 19.327 ± 0.050 19.683 ± 0.061 15.854 ± 0.011 16.552 ± 0.017 19.268 ± 0.034 17.790 ± 0.013 19.740 ± 0.077 16.770 ± 0.020 12.960 ± 0.020 16.150 ± 0.016 17.474 ± 0.025 18.795 ± 0.044 17.544 ± 0.027 18.077 ± 0.016 18.789 ± 0.074 20.174 ± 0.082 19.876 ± 0.088 17.791 ± 0.041 19.279 ± 0.044 16.909 ± 0.019 19.487 ± 0.058 18.359 ± 0.038 18.965 ± 0.036 17.084 ± 0.010 19.030 ± 0.062 17.599 ± 0.032

H ­ Ks (mag) 0.358 ± 0.066 0.227 ± 0.030 0.236 ± 0.033 0.371 ± 0.035 0.260 ± 0.044 0.263 ± 0.033 0.243 ± 0.026 0.244 ± 0.027 0.442 ± 0.138 0.428 ± 0.073 0.361 ± 0.041 0.469 ± 0.098 0.256 ± 0.029 0.152 ± 0.045 0.196 ± 0.135 0.131 ± 0.016 0.190 ± 0.017 0.250 ± 0.028 0.456 ± 0.084 0.287 ± 0.026 0.275 ± 0.055 0.340 ± 0.050 0.307 ± 0.058 0.193 ± 0.024 0.308 ± 0.045 0.411 ± 0.039 0.266 ± 0.019 0.348 ± 0.087 0.432 ± 0.067 1.047 ± 0.077 0.301 ± 0.046 0.315 ± 0.030 0.117 ± 0.019 0.370 ± 0.061 0.499 ± 0.032 0.332 ± 0.178 0.397 ± 0.048 0.344 ± 0.020 0.243 ± 0.033 0.419 ± 0.076 0.462 ± 0.089 0.242 ± 0.015 0.254 ± 0.033 0.481 ± 0.052 0.360 ± 0.029 0.539 ± 0.101 0.174 ± 0.034 0.198 ± 0.031 0.275 ± 0.024 0.209 ± 0.042 0.521 ± 0.054 0.275 ± 0.040 0.388 ± 0.026 0.500 ± 0.090 0.292 ± 0.125 0.522 ± 0.099 0.266 ± 0.067 0.555 ± 0.055 0.297 ± 0.031 0.434 ± 0.079 0.337 ± 0.043 0.506 ± 0.048 0.279 ± 0.016 0.256 ± 0.091 0.278 ± 0.048


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 13.79 05 17 13.26 05 17 21.55 05 17 28.94 05 17 21.15 05 16 57.89 05 17 00.54 05 17 14.37 05 17 07.52 05 17 17.87 05 17 05.82 05 17 10.24 05 17 12.37 05 17 14.47 05 17 02.92 05 17 21.37 05 17 12.90 05 17 11.93 05 17 24.54 05 17 15.69 05 17 12.68 05 17 26.09 05 17 14.35 05 17 13.82 05 17 13.09 05 17 15.86 05 17 27.29 05 17 12.02 05 17 15.23 05 17 19.60 05 16 57.94 05 17 07.11 05 17 12.53 05 17 15.05 05 16 58.48 05 17 19.43 05 17 11.02 05 17 16.60 05 17 29.00 05 17 15.82 05 17 07.05 05 17 11.73 05 17 10.09 05 17 11.55 05 17 13.83 05 17 16.42 05 17 18.13 05 17 13.99 05 17 14.25 05 17 14.96 05 17 08.60 05 17 12.59 05 16 59.68 05 17 13.91 05 17 06.00 05 17 13.68 05 17 13.73 05 17 29.27 05 17 12.43 05 17 07.26 05 17 18.55 05 17 19.71 05 17 19.56 05 17 17.15 05 17 18.32 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 21 33.5 21 33.5 21 33.9 21 34.9 21 37.0 21 36.8 21 37.3 21 37.9 21 38.0 21 38.8 21 38.8 21 38.9 21 40.9 21 41.3 21 41.7 21 42.7 21 43.9 21 44.8 21 45.0 21 46.2 21 48.4 21 48.6 21 49.5 21 49.8 21 49.9 21 51.2 21 51.9 21 52.4 21 52.5 21 53.2 21 53.9 21 54.9 21 55.3 21 55.7 21 56.2 21 57.6 21 57.9 21 59.8 22 03.7 22 04.0 22 04.1 22 04.4 22 05.8 22 07.0 22 07.3 22 07.7 22 08.3 22 08.5 22 11.2 22 12.8 22 12.8 22 14.8 22 15.0 22 18.3 22 18.9 22 19.5 22 20.1 22 19.6 22 20.2 22 20.6 22 21.0 22 21.5 22 22.8 22 23.5 22 25.1 H (mag) 17.756 ± 0.016 15.728 ± 0.006 19.060 ± 0.060 15.455 ± 0.017 19.571 ± 0.081 18.026 ± 0.041 17.857 ± 0.038 18.033 ± 0.030 19.446 ± 0.083 17.698 ± 0.017 19.729 ± 0.096 18.507 ± 0.032 16.198 ± 0.007 18.174 ± 0.027 17.216 ± 0.019 18.955 ± 0.057 17.174 ± 0.017 14.402 ± 0.006 16.469 ± 0.017 19.698 ± 0.091 17.325 ± 0.017 15.982 ± 0.021 19.224 ± 0.052 18.084 ± 0.026 18.758 ± 0.048 18.501 ± 0.032 17.888 ± 0.043 15.065 ± 0.017 18.840 ± 0.046 15.960 ± 0.009 16.768 ± 0.027 18.614 ± 0.041 18.593 ± 0.029 18.982 ± 0.044 17.027 ± 0.023 16.531 ± 0.010 19.164 ± 0.078 16.861 ± 0.011 13.640 ± 0.018 19.580 ± 0.068 16.602 ± 0.011 17.307 ± 0.013 15.724 ± 0.006 19.356 ± 0.075 16.870 ± 0.013 19.392 ± 0.056 15.233 ± 0.023 18.142 ± 0.059 18.382 ± 0.026 18.109 ± 0.026 19.292 ± 0.076 18.253 ± 0.031 19.137 ± 0.097 15.720 ± 0.009 19.630 ± 0.080 11.007 ± 0.020 11.366 ± 0.020 16.978 ± 0.029 15.920 ± 0.008 19.008 ± 0.054 17.370 ± 0.038 15.811 ± 0.008 18.019 ± 0.032 19.001 ± 0.053 18.829 ± 0.050 Ks (mag) 18.070 ± 0.017 15.979 ± 0.006 19.329 ± 0.059 15.698 ± 0.015 20.090 ± 0.120 18.230 ± 0.042 18.092 ± 0.030 18.369 ± 0.024 19.671 ± 0.075 18.158 ± 0.018 20.164 ± 0.120 19.058 ± 0.028 17.500 ± 0.012 18.815 ± 0.038 17.471 ± 0.015 19.338 ± 0.070 18.179 ± 0.020 15.903 ± 0.007 16.677 ± 0.019 20.216 ± 0.106 17.738 ± 0.013 16.194 ± 0.015 19.767 ± 0.073 18.785 ± 0.025 19.351 ± 0.047 19.002 ± 0.029 18.200 ± 0.046 16.051 ± 0.011 19.451 ± 0.049 16.302 ± 0.006 16.892 ± 0.016 18.983 ± 0.045 19.029 ± 0.036 19.361 ± 0.056 17.262 ± 0.017 16.922 ± 0.010 19.749 ± 0.075 17.350 ± 0.010 13.900 ± 0.016 19.890 ± 0.103 17.058 ± 0.010 17.820 ± 0.014 15.931 ± 0.005 19.537 ± 0.059 17.372 ± 0.010 19.824 ± 0.092 15.448 ± 0.024 18.957 ± 0.033 19.121 ± 0.038 18.438 ± 0.020 19.778 ± 0.066 19.230 ± 0.042 19.956 ± 0.167 18.408 ± 0.032 20.128 ± 0.110 12.409 ± 0.012 14.548 ± 0.031 17.184 ± 0.020 16.739 ± 0.010 19.380 ± 0.056 17.605 ± 0.036 16.064 ± 0.008 18.430 ± 0.033 19.468 ± 0.050 19.197 ± 0.052 H ­ Ks (mag) 0.314 ± 0.023 0.251 ± 0.008 0.269 ± 0.084 0.243 ± 0.023 0.519 ± 0.145 0.204 ± 0.059 0.235 ± 0.048 0.336 ± 0.038 0.225 ± 0.112 0.460 ± 0.025 0.435 ± 0.154 0.551 ± 0.043 1.302 ± 0.014 0.641 ± 0.047 0.255 ± 0.024 0.383 ± 0.090 1.005 ± 0.026 1.501 ± 0.009 0.208 ± 0.025 0.518 ± 0.140 0.413 ± 0.021 0.212 ± 0.026 0.543 ± 0.090 0.701 ± 0.036 0.593 ± 0.067 0.501 ± 0.043 0.312 ± 0.063 0.986 ± 0.020 0.611 ± 0.067 0.342 ± 0.011 0.124 ± 0.031 0.369 ± 0.061 0.436 ± 0.046 0.379 ± 0.071 0.235 ± 0.029 0.391 ± 0.014 0.585 ± 0.108 0.489 ± 0.015 0.260 ± 0.024 0.310 ± 0.123 0.456 ± 0.015 0.513 ± 0.019 0.207 ± 0.008 0.181 ± 0.095 0.502 ± 0.016 0.432 ± 0.108 0.215 ± 0.033 0.815 ± 0.068 0.739 ± 0.046 0.329 ± 0.033 0.486 ± 0.101 0.977 ± 0.052 0.819 ± 0.193 2.688 ± 0.033 0.498 ± 0.136 1.402 ± 0.023 3.182 ± 0.037 0.206 ± 0.035 0.819 ± 0.013 0.372 ± 0.078 0.235 ± 0.052 0.253 ± 0.011 0.411 ± 0.046 0.467 ± 0.073 0.368 ± 0.072

35


36 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 12.72 05 17 03.13 05 17 12.82 05 17 13.98 05 17 11.01 05 17 12.00 05 17 11.06 05 17 07.33 05 17 27.87 05 17 22.36 05 17 01.19 05 17 14.79 05 17 02.28 05 16 57.83 05 17 15.98 05 17 02.49 05 17 08.93 05 17 04.30 05 17 07.03 05 17 10.93 05 16 59.03 05 16 58.24 05 17 26.06 05 17 25.40 05 17 14.90 05 17 25.89 05 17 18.03 05 17 25.96 05 17 24.76 05 17 12.10 05 16 57.76 05 17 06.69 05 17 16.95 05 17 26.82 05 17 15.80 05 17 05.88 05 17 20.78 05 17 14.97 05 17 24.14 05 17 06.77 05 17 27.56 05 17 14.30 05 17 04.89 05 17 01.02 05 17 20.80 05 17 19.46 05 16 57.82 05 16 57.80 05 17 11.89 05 16 59.55 05 16 57.91 05 17 22.74 05 17 02.21 05 17 23.90 05 17 13.41 05 17 10.76 05 17 01.03 05 17 19.44 05 17 21.13 05 17 03.13 05 17 22.67 05 17 28.10 05 17 12.84 05 16 58.12 05 17 03.97

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 22 25.5 22 25.5 22 26.6 22 27.1 22 28.9 22 30.1 22 30.4 22 30.5 22 30.9 22 32.6 22 32.6 22 33.5 22 33.4 22 34.1 22 34.9 22 39.3 22 43.0 22 43.3 22 46.0 22 47.7 22 48.1 22 48.4 22 49.9 22 52.6 22 53.5 22 55.0 22 55.3 22 56.7 22 58.1 22 58.4 22 58.4 22 59.1 23 00.2 23 00.8 23 01.0 23 01.2 23 02.2 23 02.7 23 02.9 23 08.9 23 10.2 23 12.4 23 14.0 23 14.1 23 16.2 23 17.7 23 19.7 23 20.3 23 20.7 23 22.1 23 22.9 23 24.0 23 27.7 23 29.5 23 31.1 23 33.0 23 34.6 23 35.8 23 35.8 23 35.6 23 36.6 23 37.3 23 38.9 23 38.9 23 39.5

H (mag) 18.676 ± 0.044 17.411 ± 0.022 16.936 ± 0.010 17.574 ± 0.017 19.209 ± 0.056 19.225 ± 0.060 19.288 ± 0.067 17.611 ± 0.021 17.979 ± 0.052 19.246 ± 0.070 18.700 ± 0.059 18.690 ± 0.042 18.623 ± 0.050 12.488 ± 0.014 16.788 ± 0.020 15.969 ± 0.017 18.840 ± 0.040 18.428 ± 0.036 18.937 ± 0.051 16.898 ± 0.011 18.810 ± 0.076 16.044 ± 0.013 18.588 ± 0.074 19.172 ± 0.127 19.041 ± 0.053 18.677 ± 0.073 16.666 ± 0.015 17.517 ± 0.040 19.258 ± 0.097 17.270 ± 0.013 14.951 ± 0.016 19.699 ± 0.096 16.823 ± 0.013 18.999 ± 0.105 19.599 ± 0.077 17.784 ± 0.019 15.847 ± 0.008 17.999 ± 0.026 16.112 ± 0.033 19.490 ± 0.085 18.775 ± 0.091 18.798 ± 0.048 18.039 ± 0.028 14.027 ± 0.012 18.848 ± 0.064 17.522 ± 0.019 18.227 ± 0.057 17.715 ± 0.038 18.420 ± 0.031 15.908 ± 0.014 18.035 ± 0.050 15.609 ± 0.031 18.930 ± 0.073 18.750 ± 0.061 19.368 ± 0.065 15.559 ± 0.010 17.917 ± 0.038 16.673 ± 0.025 19.816 ± 0.103 18.029 ± 0.040 18.840 ± 0.062 15.843 ± 0.024 19.311 ± 0.068 18.154 ± 0.039 16.367 ± 0.051

Ks (mag) 19.660 ± 0.053 17.781 ± 0.020 17.233 ± 0.010 18.177 ± 0.018 19.969 ± 0.087 19.638 ± 0.050 19.717 ± 0.076 17.877 ± 0.016 18.248 ± 0.041 19.578 ± 0.069 18.998 ± 0.060 19.143 ± 0.040 18.891 ± 0.056 12.740 ± 0.008 17.198 ± 0.012 16.168 ± 0.009 19.476 ± 0.056 18.836 ± 0.028 19.366 ± 0.045 17.264 ± 0.010 19.114 ± 0.065 16.189 ± 0.007 18.745 ± 0.084 19.253 ± 0.084 19.490 ± 0.063 19.156 ± 0.097 16.921 ± 0.014 17.727 ± 0.029 19.683 ± 0.106 17.639 ± 0.013 15.064 ± 0.008 19.861 ± 0.086 17.035 ± 0.010 19.436 ± 0.138 19.907 ± 0.092 18.094 ± 0.020 16.048 ± 0.009 18.330 ± 0.026 16.277 ± 0.015 20.009 ± 0.095 19.144 ± 0.082 19.216 ± 0.047 18.369 ± 0.028 14.141 ± 0.005 19.733 ± 0.074 17.843 ± 0.020 18.578 ± 0.054 17.912 ± 0.042 18.670 ± 0.029 16.057 ± 0.008 18.283 ± 0.042 15.928 ± 0.014 19.545 ± 0.113 19.102 ± 0.059 19.711 ± 0.052 15.725 ± 0.007 18.328 ± 0.036 16.847 ± 0.021 20.143 ± 0.139 18.319 ± 0.026 18.990 ± 0.050 16.041 ± 0.016 19.747 ± 0.069 18.516 ± 0.059 16.565 ± 0.031

H ­ Ks (mag) 0.984 ± 0.069 0.370 ± 0.030 0.297 ± 0.014 0.603 ± 0.025 0.760 ± 0.103 0.413 ± 0.078 0.429 ± 0.101 0.266 ± 0.026 0.269 ± 0.066 0.332 ± 0.098 0.298 ± 0.084 0.453 ± 0.058 0.268 ± 0.075 0.252 ± 0.016 0.410 ± 0.023 0.199 ± 0.019 0.636 ± 0.069 0.408 ± 0.046 0.429 ± 0.068 0.366 ± 0.015 0.304 ± 0.100 0.145 ± 0.015 0.157 ± 0.112 0.081 ± 0.152 0.449 ± 0.082 0.479 ± 0.121 0.255 ± 0.021 0.210 ± 0.049 0.425 ± 0.144 0.369 ± 0.018 0.113 ± 0.018 0.162 ± 0.129 0.212 ± 0.016 0.437 ± 0.173 0.308 ± 0.120 0.310 ± 0.028 0.201 ± 0.012 0.331 ± 0.037 0.165 ± 0.036 0.519 ± 0.127 0.369 ± 0.122 0.418 ± 0.067 0.330 ± 0.040 0.114 ± 0.013 0.885 ± 0.098 0.321 ± 0.028 0.351 ± 0.079 0.197 ± 0.057 0.250 ± 0.042 0.149 ± 0.016 0.248 ± 0.065 0.319 ± 0.034 0.615 ± 0.135 0.352 ± 0.085 0.343 ± 0.083 0.166 ± 0.012 0.411 ± 0.052 0.174 ± 0.033 0.327 ± 0.173 0.290 ± 0.048 0.150 ± 0.080 0.198 ± 0.029 0.436 ± 0.097 0.362 ± 0.071 0.198 ± 0.060


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 27.29 05 17 22.56 05 17 12.61 05 17 15.30 05 17 00.31 05 17 27.30 05 17 25.36 05 17 26.75 05 17 01.63 05 17 18.97 05 17 01.27 05 17 04.30 05 17 20.53 05 17 27.41 05 17 07.94 05 17 19.93 05 17 20.49 05 17 18.43 05 17 09.69 05 17 09.22 05 17 18.24 05 17 15.46 05 17 25.49 05 17 04.11 05 17 04.08 05 17 02.52 05 17 16.45 05 17 25.31 05 17 05.30 05 17 12.80 05 17 18.51 05 17 18.82 05 17 19.37 05 17 27.02 05 17 29.84 05 17 22.72 05 17 22.39 05 17 01.22 05 17 14.33 05 17 26.40 05 17 29.74 05 17 10.88 05 17 06.16 05 17 19.40 05 17 17.76 05 17 21.72 05 17 14.10 05 17 09.85 05 17 06.80 05 17 17.42 05 17 12.44 05 17 17.06 05 17 17.54 05 17 03.06 05 17 24.76 05 17 22.00 05 17 18.79 05 17 12.02 05 17 24.68 05 17 24.18 05 17 28.95 05 17 27.05 05 17 02.85 05 17 07.35 05 17 10.35 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 23 40.5 23 42.8 23 44.0 23 46.0 23 46.2 23 47.6 23 48.2 23 50.7 23 51.2 23 52.7 23 52.8 23 53.0 23 53.9 23 54.0 23 54.1 23 54.6 23 54.9 23 55.5 23 56.2 23 56.7 23 57.3 23 57.5 23 59.2 23 59.8 24 00.1 23 59.9 24 01.9 24 02.3 24 03.8 24 05.4 24 05.5 24 08.3 24 09.1 24 09.8 24 10.5 24 11.8 24 12.5 24 12.4 24 14.3 24 16.6 24 16.7 24 17.1 24 18.6 24 21.1 24 25.4 24 25.6 24 27.0 20 08.6 20 11.6 20 16.5 20 20.5 20 21.2 20 23.2 20 26.0 20 27.1 20 29.6 20 33.1 20 40.6 20 40.8 20 41.1 20 44.1 20 52.7 20 58.5 20 58.8 21 07.0 H (mag) 17.007 ± 0.034 19.211 ± 0.077 17.331 ± 0.014 18.981 ± 0.056 18.632 ± 0.073 16.968 ± 0.038 15.398 ± 0.018 18.994 ± 0.105 19.207 ± 0.101 15.944 ± 0.016 17.258 ± 0.029 17.471 ± 0.065 17.674 ± 0.026 16.475 ± 0.031 17.315 ± 0.013 16.660 ± 0.024 19.112 ± 0.074 19.005 ± 0.050 17.283 ± 0.016 19.168 ± 0.053 17.282 ± 0.018 17.931 ± 0.028 18.331 ± 0.065 16.151 ± 0.022 16.074 ± 0.025 16.037 ± 0.069 18.785 ± 0.068 15.944 ± 0.023 18.625 ± 0.073 18.944 ± 0.072 18.511 ± 0.055 18.643 ± 0.043 15.365 ± 0.027 17.566 ± 0.056 17.025 ± 0.047 18.067 ± 0.044 17.337 ± 0.042 16.106 ± 0.022 15.659 ± 0.025 19.534 ± 0.332 17.987 ± 0.085 16.749 ± 0.016 16.275 ± 0.036 17.334 ± 0.056 14.197 ± 0.013 16.992 ± 0.040 16.229 ± 0.021 18.009 ± 0.047 13.114 ± 0.039 16.658 ± 0.023 15.804 ± 0.023 17.995 ± 0.045 17.324 ± 0.034 16.667 ± 0.044 17.369 ± 0.044 15.364 ± 0.036 15.929 ± 0.024 12.847 ± 0.030 14.683 ± 0.048 17.723 ± 0.062 13.613 ± 0.020 13.362 ± 0.019 11.371 ± 0.037 15.297 ± 0.009 15.179 ± 0.010 Ks (mag) 17.252 ± 0.024 19.553 ± 0.066 17.617 ± 0.009 19.398 ± 0.057 18.828 ± 0.058 17.191 ± 0.020 15.525 ± 0.012 19.193 ± 0.095 19.363 ± 0.089 16.103 ± 0.012 17.451 ± 0.024 17.618 ± 0.054 17.908 ± 0.016 16.635 ± 0.020 17.568 ± 0.013 16.840 ± 0.011 19.192 ± 0.049 19.312 ± 0.050 17.444 ± 0.020 19.533 ± 0.063 17.584 ± 0.011 18.117 ± 0.022 18.501 ± 0.053 16.190 ± 0.019 16.332 ± 0.024 16.828 ± 0.049 19.089 ± 0.047 16.178 ± 0.021 18.744 ± 0.052 19.634 ± 0.076 18.785 ± 0.040 18.783 ± 0.038 15.536 ± 0.006 17.854 ± 0.063 17.237 ± 0.029 18.109 ± 0.040 17.453 ± 0.029 16.273 ± 0.021 15.818 ± 0.023 19.691 ± 0.234 18.293 ± 0.055 16.678 ± 0.019 16.483 ± 0.020 17.484 ± 0.034 14.273 ± 0.014 17.231 ± 0.032 16.431 ± 0.014 18.387 ± 0.042 13.386 ± 0.021 16.852 ± 0.043 16.044 ± 0.019 18.334 ± 0.035 17.584 ± 0.034 16.930 ± 0.021 17.547 ± 0.049 15.776 ± 0.037 16.163 ± 0.024 13.004 ± 0.022 14.873 ± 0.035 18.063 ± 0.045 13.760 ± 0.015 13.529 ± 0.013 11.682 ± 0.025 15.492 ± 0.010 15.374 ± 0.010 H ­ Ks (mag) 0.245 ± 0.042 0.342 ± 0.101 0.286 ± 0.017 0.417 ± 0.080 0.196 ± 0.093 0.223 ± 0.043 0.127 ± 0.022 0.199 ± 0.142 0.156 ± 0.135 0.159 ± 0.020 0.193 ± 0.038 0.147 ± 0.085 0.234 ± 0.031 0.160 ± 0.037 0.253 ± 0.018 0.180 ± 0.026 0.080 ± 0.089 0.307 ± 0.071 0.161 ± 0.026 0.365 ± 0.082 0.302 ± 0.021 0.186 ± 0.036 0.170 ± 0.084 0.039 ± 0.029 0.258 ± 0.035 0.791 ± 0.085 0.304 ± 0.083 0.234 ± 0.031 0.119 ± 0.090 0.690 ± 0.105 0.274 ± 0.068 0.140 ± 0.057 0.171 ± 0.028 0.288 ± 0.084 0.212 ± 0.055 0.042 ± 0.059 0.116 ± 0.051 0.167 ± 0.030 0.159 ± 0.034 0.157 ± 0.406 0.306 ± 0.101 -0.071 ± 0.025 0.208 ± 0.041 0.150 ± 0.066 0.076 ± 0.019 0.239 ± 0.051 0.202 ± 0.025 0.378 ± 0.063 0.272 ± 0.044 0.194 ± 0.049 0.240 ± 0.030 0.339 ± 0.057 0.260 ± 0.048 0.263 ± 0.049 0.178 ± 0.066 0.412 ± 0.052 0.234 ± 0.034 0.157 ± 0.037 0.190 ± 0.059 0.340 ± 0.077 0.147 ± 0.025 0.167 ± 0.023 0.311 ± 0.045 0.195 ± 0.013 0.195 ± 0.014

37


38 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 14.18 05 17 09.45 05 17 20.29 05 17 28.03 05 17 16.08 05 17 24.18 05 17 13.55 05 16 58.57 05 17 09.54 05 17 05.73 05 17 22.32 05 17 04.22 05 17 03.62 05 17 01.81 05 17 17.68 05 17 18.15 05 17 12.20 05 17 12.74 05 17 14.38 05 17 23.07 05 17 12.67 05 16 57.90 05 17 14.55 05 17 12.85 05 17 14.38 05 17 13.74 05 17 12.61 05 17 13.02 05 17 15.40 05 17 13.09 05 17 14.12 05 17 28.10 05 17 09.35 05 17 14.53 05 16 58.15 05 17 07.28 05 17 18.55 05 17 28.62 05 17 00.79 05 17 02.84 05 17 13.62 05 17 29.49 05 17 23.43 05 17 17.05 05 17 09.69 05 17 22.48 05 17 29.17 05 17 25.86 05 16 59.19 05 17 09.21 05 17 00.76 05 17 25.09 05 17 08.36 05 17 09.61 05 17 16.17 05 17 01.92 05 16 58.22 05 17 17.16 05 17 28.67 05 17 00.71 05 17 22.42 05 17 10.32 05 17 08.96 05 17 17.21 05 17 09.67

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 21 12.1 21 13.3 21 13.8 21 13.9 21 22.2 21 23.6 21 29.7 21 30.3 21 32.2 21 33.0 21 36.8 21 39.9 21 40.2 21 49.1 21 49.9 21 55.7 21 55.6 21 56.3 22 00.6 22 01.4 22 04.7 22 04.9 22 14.7 22 18.9 22 21.9 22 23.5 22 26.1 22 26.5 22 30.3 22 30.7 22 32.3 22 36.8 22 44.6 22 48.7 22 54.2 22 58.2 23 07.0 23 17.0 23 21.5 23 24.2 23 28.8 23 29.4 23 31.8 23 39.0 23 42.5 23 46.0 23 54.8 23 54.8 23 59.6 24 01.1 24 01.7 24 05.1 24 06.2 24 09.7 24 11.1 24 13.2 24 15.4 24 16.1 24 20.7 24 20.8 24 25.5 20 14.9 20 17.0 20 19.8 20 21.4

H (mag) 14.967 ± 0.008 15.877 ± 0.014 19.526 ± 0.089 14.268 ± 0.019 18.533 ± 0.027 17.822 ± 0.036 19.594 ± 0.077 17.738 ± 0.035 17.598 ± 0.016 18.795 ± 0.047 18.753 ± 0.058 18.454 ± 0.042 19.709 ± 0.103 16.057 ± 0.016 16.530 ± 0.010 15.978 ± 0.022 13.754 ± 0.008 15.548 ± 0.006 18.022 ± 0.025 15.952 ± 0.010 14.668 ± 0.033 17.168 ± 0.024 17.868 ± 0.018 11.294 ± 0.005 15.101 ± 0.006 15.487 ± 0.011 17.371 ± 0.012 16.797 ± 0.015 16.543 ± 0.016 16.758 ± 0.014 18.739 ± 0.036 18.272 ± 0.061 19.771 ± 0.111 18.308 ± 0.031 18.620 ± 0.063 15.031 ± 0.006 12.584 ± 0.017 15.407 ± 0.024 18.872 ± 0.085 13.946 ± 0.042 18.783 ± 0.041 15.288 ± 0.029 17.577 ± 0.050 17.458 ± 0.029 19.322 ± 0.066 19.018 ± 0.075 18.258 ± 0.069 18.810 ± 0.111 15.632 ± 0.043 16.130 ± 0.010 14.127 ± 0.032 18.847 ± 0.097 18.997 ± 0.055 16.556 ± 0.015 18.095 ± 0.050 16.446 ± 0.026 14.121 ± 0.021 15.392 ± 0.018 19.743 ± 0.271 18.146 ± 0.075 20.239 ± 0.453 16.397 ± 0.039 17.194 ± 0.027 16.507 ± 0.028 16.464 ± 0.029

Ks (mag) 15.258 ± 0.007 16.096 ± 0.011 19.792 ± 0.072 14.476 ± 0.014 19.060 ± 0.040 18.454 ± 0.030 20.213 ± 0.113 18.041 ± 0.042 18.065 ± 0.018 19.181 ± 0.049 19.240 ± 0.049 19.505 ± 0.076 20.037 ± 0.107 16.219 ± 0.011 16.843 ± 0.010 16.277 ± 0.012 14.836 ± 0.007 16.194 ± 0.006 18.662 ± 0.027 16.226 ± 0.010 15.208 ± 0.020 17.377 ± 0.019 18.514 ± 0.016 11.390 ± 0.005 16.227 ± 0.006 16.776 ± 0.009 18.271 ± 0.021 17.576 ± 0.011 16.724 ± 0.009 17.541 ± 0.013 19.332 ± 0.042 18.416 ± 0.054 20.123 ± 0.113 18.670 ± 0.022 19.017 ± 0.055 15.196 ± 0.005 12.724 ± 0.009 15.579 ± 0.014 19.571 ± 0.110 14.127 ± 0.015 19.280 ± 0.054 15.445 ± 0.017 17.744 ± 0.025 17.713 ± 0.023 19.717 ± 0.064 19.351 ± 0.057 18.455 ± 0.063 18.840 ± 0.081 15.743 ± 0.029 16.332 ± 0.008 14.255 ± 0.020 19.367 ± 0.124 19.534 ± 0.059 16.618 ± 0.015 18.201 ± 0.039 16.534 ± 0.018 14.236 ± 0.019 15.492 ± 0.010 18.771 ± 0.120 18.259 ± 0.054 20.230 ± 0.380 16.648 ± 0.028 17.411 ± 0.022 16.810 ± 0.028 16.720 ± 0.021

H ­ Ks (mag) 0.291 ± 0.011 0.219 ± 0.018 0.266 ± 0.114 0.208 ± 0.024 0.527 ± 0.048 0.632 ± 0.047 0.619 ± 0.137 0.303 ± 0.055 0.467 ± 0.024 0.386 ± 0.068 0.487 ± 0.076 1.051 ± 0.087 0.328 ± 0.149 0.162 ± 0.019 0.313 ± 0.014 0.299 ± 0.025 1.082 ± 0.011 0.646 ± 0.008 0.640 ± 0.037 0.274 ± 0.014 0.540 ± 0.039 0.209 ± 0.031 0.646 ± 0.024 0.096 ± 0.007 1.126 ± 0.008 1.289 ± 0.014 0.900 ± 0.024 0.779 ± 0.019 0.181 ± 0.018 0.783 ± 0.019 0.593 ± 0.055 0.144 ± 0.081 0.352 ± 0.158 0.362 ± 0.038 0.397 ± 0.084 0.165 ± 0.008 0.140 ± 0.019 0.172 ± 0.028 0.699 ± 0.139 0.181 ± 0.045 0.497 ± 0.068 0.157 ± 0.034 0.167 ± 0.056 0.255 ± 0.037 0.395 ± 0.092 0.333 ± 0.094 0.197 ± 0.093 0.030 ± 0.137 0.111 ± 0.052 0.202 ± 0.013 0.128 ± 0.038 0.520 ± 0.157 0.537 ± 0.081 0.062 ± 0.021 0.106 ± 0.063 0.088 ± 0.032 0.115 ± 0.028 0.100 ± 0.021 -0.972 ± 0.296 0.113 ± 0.092 -0.009 ± 0.591 0.251 ± 0.048 0.217 ± 0.035 0.303 ± 0.040 0.256 ± 0.036


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 16.77 05 17 24.09 05 17 23.48 05 17 08.79 05 17 18.91 05 17 09.83 05 17 28.08 05 17 23.26 05 17 14.40 05 17 25.42 05 17 24.90 05 17 14.32 05 17 21.41 05 17 23.24 05 17 14.13 05 17 17.22 05 17 13.27 05 17 12.52 05 17 30.03 05 17 03.07 05 17 10.42 05 17 24.05 05 17 17.24 05 17 23.22 05 17 02.51 05 16 59.24 05 17 11.90 05 16 59.51 05 17 10.82 05 17 24.12 05 17 03.03 05 17 12.57 05 17 12.36 05 17 12.84 05 16 58.37 05 17 18.43 05 17 10.42 05 17 03.86 05 17 02.68 05 17 29.62 05 17 15.57 05 17 10.52 05 17 23.70 05 17 10.55 05 17 04.66 05 17 11.74 05 17 13.64 05 17 24.79 05 17 23.26 05 17 21.85 05 17 27.40 05 17 10.24 05 17 09.96 05 17 14.64 05 17 13.62 05 17 13.75 05 17 24.63 05 17 04.21 05 17 22.89 05 17 24.40 05 17 23.41 05 17 03.42 05 17 13.75 05 17 04.28 05 17 12.85 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 20 25.4 20 27.0 20 33.6 20 35.4 20 39.5 20 44.2 20 46.5 21 28.5 21 33.8 21 48.8 21 49.9 22 02.1 22 02.2 22 04.4 22 18.0 22 19.2 22 22.3 22 35.7 23 02.6 23 32.2 23 42.0 23 47.3 23 48.1 23 56.9 24 07.0 24 07.4 24 15.4 24 15.6 24 27.5 20 09.9 20 39.8 21 48.0 22 19.4 22 35.0 22 40.6 23 29.5 23 44.9 23 57.6 23 59.3 23 59.6 24 04.1 24 09.5 24 12.6 24 18.0 24 22.4 21 55.8 22 25.6 23 45.2 23 46.3 23 59.3 24 03.4 24 08.0 20 21.8 22 08.1 22 21.9 22 22.6 23 30.5 20 24.6 21 22.4 20 22.8 20 19.7 24 00.9 22 21.2 23 59.8 22 18.2 H (mag) 15.236 ± 0.034 17.442 ± 0.062 15.660 ± 0.049 14.743 ± 0.024 16.538 ± 0.024 17.529 ± 0.047 13.433 ± 0.019 18.842 ± 0.067 19.154 ± 0.053 17.490 ± 0.039 17.548 ± 0.116 16.896 ± 0.024 17.096 ± 0.015 14.978 ± 0.030 16.961 ± 0.017 18.535 ± 0.043 18.714 ± 0.041 17.961 ± 0.064 14.630 ± 0.047 18.852 ± 0.061 15.392 ± 0.018 18.057 ± 0.063 16.730 ± 0.035 19.167 ± 0.077 16.912 ± 0.050 16.544 ± 0.055 15.953 ± 0.034 16.844 ± 0.032 13.966 ± 0.019 17.644 ± 0.072 16.655 ± 0.049 18.215 ± 0.073 17.989 ± 0.026 17.357 ± 0.020 15.719 ± 0.021 13.688 ± 0.028 14.488 ± 0.021 18.353 ± 0.080 16.006 ± 0.048 16.675 ± 0.041 14.552 ± 0.029 13.900 ± 0.025 17.866 ± 0.067 11.901 ± 0.015 12.802 ± 0.027 17.485 ± 0.049 17.316 ± 0.046 14.813 ± 0.045 15.357 ± 0.053 13.687 ± 0.048 14.908 ± 0.036 13.874 ± 0.031 15.094 ± 0.029 19.294 ± 0.071 16.016 ± 0.058 16.084 ± 0.058 17.521 ± 0.055 18.124 ± 0.069 18.159 ± 0.029 17.896 ± 0.080 19.444 ± 0.106 18.565 ± 0.076 14.992 ± 0.114 17.960 ± 0.066 14.121 ± 0.009 Ks (mag) 15.462 ± 0.034 17.606 ± 0.049 15.945 ± 0.039 14.937 ± 0.016 16.851 ± 0.019 17.793 ± 0.044 13.571 ± 0.014 18.481 ± 0.104 20.107 ± 0.097 17.683 ± 0.032 18.167 ± 0.058 17.923 ± 0.027 17.490 ± 0.015 15.213 ± 0.030 17.904 ± 0.019 18.959 ± 0.031 19.271 ± 0.042 18.140 ± 0.051 14.926 ± 0.038 19.255 ± 0.058 15.638 ± 0.013 18.147 ± 0.039 17.303 ± 0.023 19.546 ± 0.062 16.968 ± 0.034 16.676 ± 0.037 16.061 ± 0.017 17.005 ± 0.028 14.046 ± 0.011 18.063 ± 0.036 16.989 ± 0.032 18.617 ± 0.057 18.528 ± 0.029 17.739 ± 0.013 15.947 ± 0.009 13.845 ± 0.023 14.616 ± 0.014 18.645 ± 0.052 16.104 ± 0.027 16.788 ± 0.029 14.681 ± 0.021 13.980 ± 0.017 17.841 ± 0.038 11.881 ± 0.007 12.965 ± 0.025 17.801 ± 0.032 18.002 ± 0.042 15.093 ± 0.033 15.478 ± 0.032 13.804 ± 0.021 15.060 ± 0.019 13.955 ± 0.020 15.253 ± 0.025 20.040 ± 0.086 16.682 ± 0.021 16.606 ± 0.014 16.832 ± 0.052 18.420 ± 0.039 18.618 ± 0.031 18.503 ± 0.043 19.878 ± 0.100 18.480 ± 0.042 15.845 ± 0.053 18.666 ± 0.041 14.238 ± 0.010 H ­ Ks (mag) 0.226 ± 0.048 0.164 ± 0.079 0.285 ± 0.063 0.194 ± 0.029 0.313 ± 0.031 0.264 ± 0.064 0.138 ± 0.024 -0.361 ± 0.124 0.953 ± 0.111 0.193 ± 0.050 0.619 ± 0.130 1.027 ± 0.036 0.394 ± 0.021 0.235 ± 0.042 0.943 ± 0.025 0.424 ± 0.053 0.557 ± 0.059 0.179 ± 0.082 0.296 ± 0.060 0.403 ± 0.084 0.246 ± 0.022 0.090 ± 0.074 0.573 ± 0.042 0.379 ± 0.099 0.056 ± 0.060 0.132 ± 0.066 0.108 ± 0.038 0.161 ± 0.043 0.080 ± 0.022 0.419 ± 0.080 0.334 ± 0.059 0.402 ± 0.093 0.539 ± 0.039 0.382 ± 0.024 0.228 ± 0.023 0.157 ± 0.036 0.128 ± 0.025 0.292 ± 0.095 0.098 ± 0.055 0.113 ± 0.050 0.129 ± 0.036 0.080 ± 0.030 -0.025 ± 0.077 -0.020 ± 0.017 0.163 ± 0.037 0.316 ± 0.059 0.686 ± 0.062 0.280 ± 0.056 0.121 ± 0.062 0.117 ± 0.052 0.152 ± 0.041 0.081 ± 0.037 0.159 ± 0.038 0.746 ± 0.112 0.666 ± 0.062 0.522 ± 0.060 -0.689 ± 0.076 0.296 ± 0.079 0.459 ± 0.042 0.607 ± 0.091 0.434 ± 0.146 -0.085 ± 0.087 0.853 ± 0.126 0.706 ± 0.078 0.117 ± 0.013

39


40 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 10.51 05 17 17.47 05 17 18.96 05 17 20.78 05 17 17.46 05 17 08.33 05 17 06.96 05 17 23.20 05 17 02.68 05 17 10.36 05 17 13.70 05 17 14.96 05 17 01.02 05 17 13.90 05 17 18.88 05 17 08.68 05 17 13.82 05 17 14.20 05 17 12.38 05 17 19.95 05 17 04.81 05 17 02.10 05 17 09.17 05 17 05.42 05 17 04.91 05 17 16.98 05 17 09.72 05 17 21.91 05 16 59.33 05 17 01.14 05 17 22.20 05 17 16.27 05 17 15.77 05 17 10.92 05 17 15.81 05 17 11.62 05 17 14.12 05 17 10.39 05 16 59.28 05 17 12.11 05 17 11.40 05 17 26.07 05 17 24.16 05 17 11.53 05 17 12.17 05 17 06.13 05 17 13.94 05 17 15.75 05 17 13.55 05 17 02.83 05 17 16.82 05 17 27.22 05 17 14.61 05 17 14.52 05 17 07.52 05 17 27.95 05 17 14.71 05 17 14.66 05 17 24.54 05 17 13.69 05 17 12.74 05 17 14.91 05 17 14.36 05 17 20.47 05 17 08.21

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 24 18.4 20 44.7 23 06.7 20 03.6 20 16.3 20 47.1 20 57.0 21 06.9 21 21.0 21 36.7 22 12.4 22 13.4 22 13.4 22 16.1 22 19.6 22 25.4 22 33.2 22 37.4 22 51.1 23 10.2 23 14.8 23 36.7 24 01.6 20 05.5 20 15.2 20 20.4 20 22.9 20 27.1 20 40.9 20 46.0 20 50.2 20 54.1 21 13.5 21 14.7 21 19.5 21 19.8 21 22.1 21 26.1 21 36.9 21 45.4 21 47.9 21 50.1 21 51.1 21 53.2 21 57.7 22 00.0 22 02.6 22 05.2 22 05.8 22 06.2 22 07.0 22 08.5 22 10.4 22 11.3 22 12.2 22 12.9 22 14.6 22 15.3 22 15.1 22 15.6 22 16.5 22 17.0 22 17.1 22 17.4 22 20.2

H (mag) 13.124 ± 0.041 9.265 ± 0.018 14.313 ± 0.067 17.285 ± 0.044 17.528 ± 0.037 19.494 ± 0.104 19.953 ± 0.130 18.935 ± 0.062 19.529 ± 0.106 19.623 ± 0.081 18.698 ± 0.036 19.429 ± 0.075 19.591 ± 0.133 17.378 ± 0.023 19.176 ± 0.049 19.931 ± 0.121 19.432 ± 0.060 18.639 ± 0.041 19.832 ± 0.089 19.686 ± 0.123 17.584 ± 0.049 19.561 ± 0.161 18.341 ± 0.043 18.607 ± 0.128 17.851 ± 0.044 19.626 ± 0.084 19.384 ± 0.066 19.279 ± 0.077 19.307 ± 0.102 19.244 ± 0.120 19.686 ± 0.095 19.852 ± 0.094 19.658 ± 0.092 19.975 ± 0.122 20.107 ± 0.135 19.650 ± 0.089 17.936 ± 0.027 19.626 ± 0.081 18.437 ± 0.066 17.925 ± 0.046 19.469 ± 0.078 18.662 ± 0.090 18.804 ± 0.066 19.244 ± 0.052 18.110 ± 0.034 19.834 ± 0.100 19.242 ± 0.053 19.331 ± 0.072 19.599 ± 0.079 19.273 ± 0.115 19.297 ± 0.079 18.895 ± 0.113 19.737 ± 0.093 18.898 ± 0.052 19.433 ± 0.075 18.683 ± 0.088 18.160 ± 0.026 18.834 ± 0.044 18.960 ± 0.082 17.559 ± 0.021 17.700 ± 0.021 19.451 ± 0.064 18.600 ± 0.036 19.659 ± 0.090 19.519 ± 0.103

Ks (mag) 13.255 ± 0.025 9.310 ± 0.026 14.499 ± 0.056 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

H ­ Ks (mag) 0.131 ± 0.048 0.045 ± 0.032 0.186 ± 0.087 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 15.28 05 16 59.40 05 17 13.07 05 17 00.84 05 17 21.32 05 17 15.47 05 17 14.41 05 17 15.20 05 17 10.89 05 17 17.89 05 17 12.85 05 17 07.23 05 17 17.02 05 17 17.40 05 17 10.23 05 17 10.14 05 17 03.55 05 17 14.67 05 17 16.64 05 17 00.59 05 17 14.21 05 17 12.34 05 17 24.99 05 17 00.62 05 17 23.97 05 17 07.84 05 17 18.32 05 17 09.00 05 17 13.22 05 16 58.29 05 17 13.58 05 17 28.99 05 17 10.78 05 17 10.79 05 17 12.78 05 16 57.93 05 17 18.17 05 16 57.49 05 17 00.08 05 17 20.04 05 17 13.91 05 17 23.23 05 17 03.42 05 17 10.72 05 17 24.94 05 17 04.34 05 17 08.93 05 17 01.06 05 17 14.87 05 17 15.25 05 17 11.89 05 17 14.90 05 17 12.99 05 17 13.72 05 17 17.82 05 17 25.58 05 17 24.60 05 17 09.70 05 17 03.33 05 17 17.15 05 17 15.83 05 17 20.02 05 17 23.27 05 17 10.87 05 17 28.18 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 22 21.9 22 21.8 22 26.0 22 26.6 22 27.0 22 28.9 22 35.9 22 36.2 22 37.4 22 40.9 22 55.8 23 05.8 23 12.8 23 14.5 23 15.4 23 16.3 23 17.2 23 32.8 23 32.9 23 34.3 23 35.9 23 39.4 23 41.0 23 47.3 23 49.8 23 51.0 24 07.2 20 16.1 21 15.2 21 30.4 22 00.9 22 06.8 22 13.6 22 16.1 22 22.5 22 44.8 22 45.6 22 49.4 23 00.2 23 12.6 23 15.8 23 40.1 23 41.7 23 43.2 24 06.4 24 14.4 20 15.9 20 47.9 21 04.7 21 15.0 21 50.0 22 06.9 22 12.7 22 17.0 23 20.7 23 22.1 23 30.2 23 32.8 23 42.5 20 08.7 21 13.9 21 18.4 21 42.6 21 50.4 21 51.0 H (mag) 19.619 ± 0.083 19.224 ± 0.108 18.833 ± 0.043 19.690 ± 0.153 19.698 ± 0.096 18.025 ± 0.036 19.192 ± 0.068 19.500 ± 0.054 19.366 ± 0.072 19.613 ± 0.101 19.922 ± 0.095 19.881 ± 0.149 19.759 ± 0.076 19.814 ± 0.080 19.578 ± 0.074 19.974 ± 0.090 19.598 ± 0.092 19.875 ± 0.099 19.332 ± 0.075 19.204 ± 0.104 19.591 ± 0.089 20.134 ± 0.158 18.853 ± 0.094 19.124 ± 0.124 17.937 ± 0.036 19.829 ± 0.102 19.766 ± 0.119 18.650 ± 0.039 19.755 ± 0.100 18.846 ± 0.076 18.961 ± 0.055 19.073 ± 0.136 20.068 ± 0.134 19.286 ± 0.068 19.682 ± 0.093 18.933 ± 0.125 19.084 ± 0.068 18.581 ± 0.106 18.923 ± 0.078 19.785 ± 0.128 19.659 ± 0.077 19.422 ± 0.096 19.243 ± 0.097 19.659 ± 0.082 18.857 ± 0.108 18.975 ± 0.092 18.952 ± 0.068 18.862 ± 0.079 20.221 ± 0.158 20.031 ± 0.125 19.184 ± 0.090 19.267 ± 0.060 19.434 ± 0.069 17.004 ± 0.056 19.683 ± 0.068 20.161 ± 0.312 17.220 ± 0.041 19.838 ± 0.085 19.529 ± 0.126 19.472 ± 0.103 19.785 ± 0.079 19.588 ± 0.115 17.954 ± 0.052 18.667 ± 0.041 19.205 ± 0.151 Ks (mag) -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- H ­ Ks (mag) -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

41


42 Table A.1. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 28.81 05 17 13.25 05 17 23.45 05 16 58.72 05 17 19.39 05 17 09.66 05 17 27.93 05 17 14.06 05 17 21.01 05 17 10.84 05 17 00.03 05 17 13.80 05 17 29.06 05 17 00.87 05 17 09.57 05 17 25.63 05 17 03.79 05 17 10.22 05 17 29.33 05 17 28.68 05 17 02.13 05 17 25.01 05 17 17.46 05 17 04.92 05 17 03.99 05 17 05.63 05 17 25.77 05 17 10.98 05 17 24.24 05 17 13.66 05 17 17.19 05 17 27.96 05 17 13.55 05 17 14.21 05 17 04.65 05 17 10.50 05 17 16.24 05 17 09.42 05 17 29.53 05 17 10.62 05 17 29.33 05 17 16.57 05 17 28.19 05 17 28.90 05 17 28.99 05 17 08.43 05 17 29.07 05 17 07.34 05 17 03.81 05 17 05.89 05 17 23.65 05 17 00.35 05 17 25.66 05 17 26.86 05 17 04.25 05 17 25.49 05 17 28.45 05 17 23.28 05 17 03.42 05 17 23.10 05 17 29.93 05 17 20.00 05 17 28.70 05 17 04.30 05 17 07.63

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 23 40.7 21 24.6 21 26.8 23 25.5 23 35.5 23 56.5 24 10.8 22 17.0 23 16.5 24 17.4 21 55.8 22 20.9 22 18.0 23 59.0 24 10.2 21 15.4 20 27.9 22 44.7 22 56.0 23 53.9 23 58.2 20 25.1 20 35.4 20 47.3 20 50.6 20 55.5 21 01.1 21 03.3 21 04.0 21 50.8 21 54.0 22 22.2 22 29.1 22 41.4 22 55.4 23 00.9 23 12.8 23 13.6 23 20.5 23 27.8 23 41.4 23 41.4 23 43.3 23 52.6 23 55.9 23 59.6 24 05.0 24 18.2 24 21.6 24 22.4 20 25.0 20 32.2 20 58.4 23 16.1 23 21.9 24 04.1 24 05.8 24 17.1 20 23.5 20 34.2 21 03.6 21 23.1 23 24.0 23 59.5 24 18.3

H (mag) 18.911 ± 0.109 18.515 ± 0.046 18.925 ± 0.075 19.354 ± 0.112 18.095 ± 0.045 18.828 ± 0.057 19.621 ± 0.310 17.691 ± 0.042 19.188 ± 0.058 17.947 ± 0.054 20.428 ± 0.415 15.052 ± 0.044 18.936 ± 0.141 19.315 ± 0.122 18.451 ± 0.087 18.638 ± 0.115 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

Ks (mag) -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 20.231 ± 0.136 20.519 ± 0.150 19.543 ± 0.174 19.266 ± 0.117 19.411 ± 0.086 20.678 ± 0.394 19.869 ± 0.093 19.876 ± 0.086 20.080 ± 0.095 20.081 ± 0.117 19.351 ± 0.120 20.499 ± 0.112 16.441 ± 0.035 20.123 ± 0.107 20.221 ± 0.092 19.537 ± 0.153 19.908 ± 0.082 18.648 ± 0.061 19.555 ± 0.058 20.287 ± 0.110 19.870 ± 0.070 20.331 ± 0.096 18.936 ± 0.098 20.330 ± 0.117 18.360 ± 0.056 19.469 ± 0.075 19.809 ± 0.175 19.223 ± 0.106 19.389 ± 0.130 19.868 ± 0.075 19.093 ± 0.118 19.358 ± 0.107 18.426 ± 0.070 18.591 ± 0.086 19.987 ± 0.129 19.810 ± 0.129 19.623 ± 0.141 20.326 ± 0.257 20.076 ± 0.107 20.372 ± 0.362 20.867 ± 0.492 18.939 ± 0.092 19.738 ± 0.082 19.803 ± 0.083 19.193 ± 0.134 20.183 ± 0.137 19.434 ± 0.130 18.369 ± 0.029 19.156 ± 0.081

H ­ Ks (mag) -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.1. Continued. RA (hh mm ss) 05 17 24.08 05 17 07.76 05 16 58.51 05 17 24.37 05 17 23.11 05 17 23.31 05 17 02.68 05 17 18.51 05 17 17.26 05 17 06.94 05 17 13.20 (dd 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 20 10.2 22 59.6 23 20.0 20 23.0 20 26.3 23 49.1 20 38.6 20 03.8 23 48.4 24 17.8 21 25.1 H (mag) -- -- -- -- -- -- -- -- -- -- -- Ks (mag) 18.194 ± 0.051 20.031 ± 0.097 18.371 ± 0.040 18.607 ± 0.064 20.235 ± 0.161 17.802 ± 0.031 19.693 ± 0.106 18.620 ± 0.133 18.091 ± 0.025 18.707 ± 0.054 19.276 ± 0.050 H ­ Ks (mag) -- -- -- -- -- -- -- -- -- -- --

43


44

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Table A.2. Coordinates and fluxes of the H2 knots belonging to Jet 1. (J2000) (hh mm ss) 05 17 14.495 05 17 14.488 05 17 14.505 05 17 14.595 05 17 14.640 05 17 14.539 05 17 14.361 05 17 14.232 O5 17 14.133 05 17 14.194 05 17 14.248 05 17 14.432 05 17 14.579 05 17 14.646 05 17 13.463 05 17 13.423 05 17 13.847 05 17 13.722 05 17 13.510 05 17 13.507 05 17 12.896 05 17 12.975 05 17 13.160 05 17 11.922 05 17 11.807 05 17 12.035 05 17 12.113 (J2000) (dd mm ss) 39 22 43.28 39 22 45.27 39 22 46.32 39 22 43.51 39 22 42.72 39 22 41.90 39 22 42.39 39 22 41.31 39 22 39.21 39 22 38.78 39 22 39.37 39 22 35.76 39 22 39.30 39 22 40.59 39 22 11.80 39 22 09.35 39 21 49.04 39 21 50.53 39 21 51.96 39 21 48.83 39 21 46.80 39 21 43.35 39 21 45.05 39 21 46.06 39 21 47.71 39 21 51.89 39 21 45.85 Flux (10-16 erg cm-2 s-1 ) 584.7±0.6 527.2±0.5 20.8±0.2 85.0±0.3 89.0±0.4 66.9±0.3 62.9±0.3 351.1±0.4 80.7±0.3 118.6±0.4 45.9±0.3 21.5±0.3 22.4±0.3 22.3±0.3 2.6±0.2 10.8±0.5 92.3±0.6 173.2±0.7 163.4±0.7 26.7±0.5 65.3±0.7 14.4±0.4 18.2±0.5 41.9±0.4 21.7±0.3 40.1±0.4 13.6±0.3

Table A.3. Coordinates and fluxes of the H2 knots belonging to Jet 2. (J2000) (hh mm ss) 05:17:13.398 05:17:13.493 05:17:13.626 05:17:13.563 05:17:13.592 05:17:13.746 05:17:13.789 05:17:13.836 05:17:13.878 05:17:13.956 05:17:14.020 05:17:13.973 05:17:14.051 05:17:13.897 (J2000) (dd mm ss) 39:22:27.89 39:22:26.33 39:22:25.50 39:22:23.34 39:22:22.56 39:22:18.50 39:22:16.12 39:22:14.67 39:22:13.11 39:22:10.97 39:22:07.75 39:22:06.39 39:22:05.20 39:22:07.08 Flux (10-16 erg cm-2 s-1 ) 39.4±0.4 115.1±0.6 19.4±0.3 27.4±0.3 21.1±0.3 18.3±0.3 9.5±0.3 11.3±0.3 11.5±0.3 16.9±0.5 83.0±0.4 156.0±0.5 10.8±0.2 37.6±0.3

Table A.4. Coordinates and fluxes of the H2 knots belonging to Jet 3. (J2000) (hh mm ss) 05 17 13.618 05 17 13.391 05 17 12.928 (J2000) (dd mm ss) 39 22 16.98 39 22 15.94 39 22 13.28 Flux (10-16 erg cm-2 s-1 ) 47.3±0.4 38.5±0.4 3.3±0.2


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.5. Coordinates, magnitudes, and colour of the sources identified in the PISCES field. The symbol "--" indicates a non-detection. RA (hh mm ss) 05 17 13.98 05 17 13.28 05 17 14.15 05 17 14.25 05 17 13.71 05 17 12.99 05 17 14.25 05 17 14.14 05 17 13.27 05 17 14.13 05 17 13.69 05 17 13.82 05 17 13.90 05 17 13.72 05 17 14.06 05 17 13.73 05 17 14.36 05 17 13.98 05 17 14.00 05 17 13.55 05 17 14.13 05 17 13.57 05 17 13.91 05 17 13.08 05 17 13.36 05 17 13.65 05 17 14.08 05 17 13.21 05 17 13.40 05 17 13.67 05 17 13.73 05 17 13.74 05 17 13.30 05 17 13.61 05 17 13.64 05 17 13.81 05 17 13.76 05 17 14.28 05 17 13.76 05 17 13.99 05 17 13.17 05 17 12.93 05 17 14.38 05 17 13.62 05 17 13.26 05 17 13.27 05 17 13.75 05 17 13.24 05 17 13.79 05 17 13.29 05 17 13.74 05 17 13.46 05 17 13.49 05 17 12.96 05 17 13.64 05 17 13.29 05 17 13.65 05 17 13.73 05 17 14.30 05 17 13.94 05 17 13.62 05 17 12.99 05 17 13.84 05 17 13.02 05 17 13.97 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 22 08.6 22 09.6 22 09.8 22 11.2 22 12.4 22 12.6 22 12.8 22 13.6 22 13.7 22 13.9 22 15.6 22 15.7 22 16.1 22 16.9 22 17.0 22 17.0 22 17.1 22 17.4 22 17.6 22 17.7 22 17.9 22 18.1 22 18.3 22 18.3 22 18.6 22 18.7 22 18.8 22 19.2 22 19.3 22 19.5 22 20.1 22 20.3 22 20.4 22 20.5 22 20.7 22 20.9 22 21.0 22 21.3 22 21.3 22 21.7 22 21.7 22 21.7 22 21.9 22 22.0 22 22.2 22 22.3 22 22.6 22 22.9 22 23.3 22 23.4 22 23.5 22 23.7 22 23.8 22 24.1 22 24.2 22 25.4 22 25.6 22 26.0 22 26.2 22 26.2 22 26.2 22 26.3 22 26.4 22 26.5 22 27.1 H (mag) 18.578 ± 0.014 19.101 ± 0.010 18.494 ± 0.008 18.443 ± 0.007 18.429 ± 0.005 19.705 ± 0.056 17.837 ± 0.004 17.793 ± 0.004 19.191 ± 0.011 17.694 ± 0.004 17.522 ± 0.003 18.777 ± 0.008 17.131 ± 0.002 17.691 ± 0.007 18.158 ± 0.005 18.007 ± 0.009 16.769 ± 0.002 17.763 ± 0.011 15.764 ± 0.002 17.325 ± 0.010 16.956 ± 0.003 18.172 ± 0.025 15.497 ± 0.001 16.675 ± 0.001 19.155 ± 0.011 16.762 ± 0.059 17.076 ± 0.003 18.485 ± 0.006 19.020 ± 0.009 11.273 ± 0.001 11.181 ± 0.002 13.359 ± 0.009 18.373 ± 0.005 17.899 ± 0.021 18.080 ± 0.049 15.467 ± 0.002 15.677 ± 0.006 18.729 ± 0.010 16.585 ± 0.006 18.924 ± 0.012 16.251 ± 0.001 19.246 ± 0.011 15.128 ± 0.002 16.174 ± 0.002 19.373 ± 0.016 18.928 ± 0.011 16.122 ± 0.002 15.813 ± 0.001 18.081 ± 0.007 17.441 ± 0.003 15.352 ± 0.001 15.961 ± 0.001 15.914 ± 0.001 18.064 ± 0.005 16.860 ± 0.002 18.034 ± 0.004 17.250 ± 0.003 18.838 ± 0.009 18.260 ± 0.007 17.800 ± 0.004 18.332 ± 0.009 18.691 ± 0.017 18.075 ± 0.005 16.701 ± 0.003 17.494 ± 0.004 Ks (mag) 19.241 ± 0.029 19.625 ± 0.037 19.227 ± 0.037 19.295 ± 0.038 20.119 ± 0.071 20.092 ± 0.054 18.901 ± 0.031 19.046 ± 0.038 20.032 ± 0.062 18.431 ± 0.020 20.137 ± 0.074 20.226 ± 0.067 19.856 ± 0.047 19.608 ± 0.052 20.072 ± 0.072 20.412 ± 0.099 18.779 ± 0.039 20.249 ± 0.083 18.229 ± 0.020 18.849 ± 0.026 18.107 ± 0.017 19.459 ± 0.063 17.930 ± 0.012 17.476 ± 0.009 19.812 ± 0.042 17.214 ± 0.036 18.901 ± 0.026 19.049 ± 0.022 19.597 ± 0.042 12.523 ± 0.003 14.933 ± 0.007 15.474 ± 0.008 19.131 ± 0.029 19.386 ± 0.060 18.464 ± 0.032 16.731 ± 0.008 16.339 ± 0.006 20.168 ± 0.076 17.512 ± 0.020 20.008 ± 0.061 17.232 ± 0.007 19.913 ± 0.049 16.452 ± 0.008 16.852 ± 0.007 19.984 ± 0.059 19.500 ± 0.033 16.470 ± 0.005 17.180 ± 0.008 18.996 ± 0.028 18.739 ± 0.022 16.594 ± 0.006 16.557 ± 0.006 16.719 ± 0.007 19.907 ± 0.046 17.408 ± 0.009 19.315 ± 0.033 17.946 ± 0.013 19.759 ± 0.061 19.127 ± 0.030 18.645 ± 0.021 19.252 ± 0.033 20.393 ± 0.098 18.751 ± 0.024 17.448 ± 0.009 17.975 ± 0.016 H ­ Ks (mag) 0.663 ± 0.032 0.524 ± 0.038 0.733 ± 0.038 0.852 ± 0.039 1.690 ± 0.071 0.387 ± 0.078 1.064 ± 0.031 1.253 ± 0.038 0.841 ± 0.063 0.737 ± 0.020 2.615 ± 0.074 1.449 ± 0.067 2.725 ± 0.047 1.917 ± 0.052 1.914 ± 0.072 2.405 ± 0.099 2.010 ± 0.039 2.486 ± 0.084 2.465 ± 0.020 1.524 ± 0.028 1.151 ± 0.017 1.287 ± 0.068 2.433 ± 0.012 0.801 ± 0.009 0.657 ± 0.043 0.452 ± 0.069 1.825 ± 0.026 0.564 ± 0.023 0.577 ± 0.043 1.250 ± 0.003 3.752 ± 0.007 2.115 ± 0.012 0.758 ± 0.029 1.487 ± 0.064 0.384 ± 0.059 1.264 ± 0.008 0.662 ± 0.008 1.439 ± 0.077 0.927 ± 0.021 1.084 ± 0.062 0.981 ± 0.007 0.667 ± 0.050 1.324 ± 0.008 0.678 ± 0.007 0.611 ± 0.061 0.572 ± 0.035 0.348 ± 0.005 1.367 ± 0.008 0.915 ± 0.029 1.298 ± 0.022 1.242 ± 0.006 0.596 ± 0.006 0.805 ± 0.007 1.843 ± 0.046 0.548 ± 0.009 1.281 ± 0.033 0.696 ± 0.013 0.921 ± 0.062 0.867 ± 0.031 0.845 ± 0.021 0.920 ± 0.034 1.702 ± 0.099 0.676 ± 0.025 0.747 ± 0.009 0.481 ± 0.016

45


46 Table A.5. Continued.

R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

RA (hh mm ss) 05 17 13.66 05 17 13.77 05 17 14.52 05 17 14.55 05 17 14.55 05 17 13.95 05 17 13.54 05 17 13.39 05 17 14.41 05 17 13.66 05 17 13.96 05 17 13.89 05 17 13.93 05 17 13.70 05 17 13.71 05 17 13.76 05 17 13.70 05 17 13.65 05 17 13.65 05 17 13.77 05 17 13.33 05 17 13.61 05 17 14.53 05 17 13.45 05 17 13.82 05 17 13.42 05 17 13.28 05 17 14.09 05 17 14.44 05 17 14.15 05 17 13.73 05 17 13.69 05 17 13.83 05 17 13.89 05 17 13.75 05 17 13.47 05 17 14.52 05 17 13.51 05 17 13.24 05 17 13.25 05 17 13.07 05 17 13.08 05 17 14.11 05 17 14.08 05 17 13.41 05 17 14.01 05 17 13.59 05 17 13.93 05 17 14.06 05 17 13.49 05 17 13.42 05 17 13.38 05 17 14.34 05 17 14.20 05 17 14.13 05 17 13.54 05 17 13.10 05 17 13.12 05 17 14.35 05 17 13.21 05 17 13.93 05 17 13.96 05 17 14.52 05 17 13.99 05 17 14.02

(dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39

Dec mm ss) 22 27.4 22 09.2 22 11.4 22 14.7 22 14.8 22 15.0 22 15.5 22 16.3 22 17.3 22 17.5 22 17.7 22 17.9 22 18.0 22 18.3 22 18.4 22 19.9 22 20.0 22 20.0 22 20.1 22 20.1 22 20.5 22 20.5 22 21.4 22 21.4 22 21.4 22 21.5 22 21.5 22 21.6 22 22.0 22 22.0 22 22.0 22 22.1 22 22.1 22 22.9 22 23.0 22 23.1 22 23.2 22 23.1 22 23.8 22 25.7 22 26.0 22 26.5 22 26.9 22 27.3 22 28.0 22 28.2 22 28.2 22 28.5 22 28.7 22 21.1 22 17.0 22 16.2 22 14.4 22 17.6 22 19.1 22 23.3 22 17.5 22 18.5 22 28.5 22 27.1 22 27.5 22 26.8 22 20.9 22 22.6 22 22.3

H (mag) 16.969 ± 0.003 19.618 ± 0.020 18.818 ± 0.009 18.372 ± 0.008 18.375 ± 0.008 20.158 ± 0.027 18.599 ± 0.026 20.077 ± 0.046 20.207 ± 0.037 19.286 ± 0.035 20.167 ± 0.048 18.872 ± 0.019 20.264 ± 0.062 18.758 ± 0.100 18.040 ± 0.057 16.632 ± 0.033 16.678 ± 0.179 16.960 ± 0.030 17.510 ± 0.107 16.031 ± 0.043 19.388 ± 0.011 18.870 ± 0.064 18.848 ± 0.012 19.304 ± 0.011 18.591 ± 0.025 19.654 ± 0.015 20.355 ± 0.032 18.881 ± 0.010 20.133 ± 0.047 20.083 ± 0.027 20.152 ± 0.109 17.890 ± 0.010 20.630 ± 0.081 19.482 ± 0.017 20.277 ± 0.041 19.875 ± 0.026 22.691 ± 0.630 19.878 ± 0.026 19.625 ± 0.020 20.467 ± 0.040 18.918 ± 0.015 22.006 ± 0.348 19.902 ± 0.024 18.252 ± 0.007 18.605 ± 0.029 20.145 ± 0.034 18.920 ± 0.030 19.688 ± 0.028 19.558 ± 0.025 20.754 ± 0.054 21.092 ± 0.065 20.656 ± 0.067 20.266 ± 0.031 20.519 ± 0.047 20.673 ± 0.057 19.322 ± 0.016 21.237 ± 0.060 22.093 ± 0.177 20.113 ± 0.042 21.253 ± 0.249 21.653 ± 0.134 20.928 ± 0.058 20.888 ± 0.065 20.919 ± 0.069 21.444 ± 0.086

Ks (mag) 17.338 ± 0.011 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

H ­ Ks (mag) 0.369 ± 0.011 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --


R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919 Table A.5. Continued. RA (hh mm ss) 05 17 13.00 05 17 13.17 05 17 13.33 05 17 13.49 05 17 13.49 05 17 13.53 05 17 13.56 05 17 14.32 05 17 14.29 05 17 14.16 05 17 12.99 05 17 13.76 05 17 13.25 05 17 13.39 05 17 13.74 05 17 13.74 05 17 13.88 05 17 14.04 05 17 14.04 05 17 12.67 05 17 13.03 05 17 14.01 05 17 12.74 05 17 14.01 05 17 13.84 05 17 13.98 05 17 13.54 05 17 13.37 05 17 13.92 05 17 14.04 05 17 12.72 05 17 12.87 05 17 13.68 05 17 12.82 05 17 13.47 05 17 13.28 05 17 12.81 05 17 12.77 05 17 13.35 05 17 13.90 05 17 12.97 05 17 13.77 05 17 13.79 (dd 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 39 Dec mm ss) 22 24.1 22 20.1 22 19.1 22 21.1 22 21.1 22 21.4 22 21.2 22 20.6 22 19.4 22 16.1 22 12.6 22 11.7 22 07.9 22 08.8 22 10.1 22 07.8 22 08.3 22 08.4 22 08.4 22 10.6 22 10.9 22 13.6 22 16.5 22 17.3 22 17.4 22 20.8 22 21.4 22 21.6 22 22.3 22 22.5 22 25.5 22 25.5 22 25.6 22 26.6 22 24.0 22 09.0 22 16.1 22 27.3 22 20.2 22 16.1 22 09.2 22 09.1 22 08.4 H (mag) 21.878 ± 0.117 22.059 ± 0.144 21.220 ± 0.072 20.721 ± 0.052 20.721 ± 0.052 20.957 ± 0.075 21.926 ± 0.326 21.398 ± 0.081 22.263 ± 0.215 20.754 ± 0.039 19.690 ± 0.055 21.560 ± 0.102 21.034 ± 0.059 21.513 ± 0.072 21.308 ± 0.066 20.720 ± 0.080 19.758 ± 0.047 19.750 ± 0.062 19.750 ± 0.062 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- Ks (mag) -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 19.074 ± 0.036 19.198 ± 0.030 21.852 ± 0.399 18.071 ± 0.012 20.888 ± 0.203 20.933 ± 0.129 20.872 ± 0.123 19.830 ± 0.062 18.964 ± 0.022 21.191 ± 0.186 20.784 ± 0.155 19.091 ± 0.042 20.637 ± 0.112 21.092 ± 0.163 16.906 ± 0.006 19.609 ± 0.098 20.577 ± 0.094 20.324 ± 0.098 19.882 ± 0.061 20.597 ± 0.089 19.848 ± 0.047 20.258 ± 0.066 20.566 ± 0.090 19.390 ± 0.042 H ­ Ks (mag) -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

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R. Cesaroni et al.: Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919

Table A.6. Continuum flux densities, S , of clumps C1 and C2 and corresponding solid angles, , over which the integration was performed. (µm) 850 500 450 350 250 160 100 70 60 25 22 21 18.7 15 12.7 12 12 12 9.9 8.9 8 4.6 4.5 3.6 3.5 3.4 2.15 1.63 1.24 (GHz) 353 599 666 856 1199 1874 2998 4283 4997 11992 13627 14075 16032 20394 23606 24776 24983 24983 30282 33685 36119 65172 66620 83275 85654 88174 136269 181692 239834 C1 (arcmin2 )
a

2.81
a

2.81 2.81 2.81
a

2.81
a a a a

0.0035
a

0.0035
a a a

0.0035 0.0035
a a

0.28 0.17
a a a a a

C2 S (Jy) (arcmin2 ) 2.86 1.09 12 2.73 13.18 -- 30 2.73 77 2.73 130 2.73 175 -- 142 2.73 140 -- 30.3 -- a 20.6 13.7 -- 10.7 -- 6.40 -- 3.8 -- 4.61 -- a 5.08 7.13 -- 1.5 -- 1.2 -- a 2.81 a 1.71 0.56 0.12 0.32 0.12 0.29 -- a 0.361 0.0555 -- 0.0148 -- 0.0058 -- a From catalogue or liter

S (Jy) 0.9 6.9 -- 16 38 61 -- 39 -- -- 4.31 -- -- -- -- -- 0.705 -- -- -- -- 0.0407 0.05 0.06 -- 0.0378 -- -- -- ature

database Di Francesco et al. (2008) Hi-GAL Di Francesco et al. (2008) Hi-GAL Hi-GAL Hi-GAL IRAS Hi-GAL IRAS IRAS WISE M SX this paper M SX this paper M SX WISE IRAS this paper this paper M SX WISE Spitzer Spitzer Ishii et al. (1998) WISE 2MASS Ks 2MASS H 2MASS J