Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://hea-www.harvard.edu/~kim/pap/N1316_2003.pdf Äàòà èçìåíåíèÿ: Mon Dec 6 20:20:37 2010 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 00:03:14 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: http www.astronomy.ru forum index.php topic 4644.0.html

The Astrophysical Journal, 586: 826­849, 2003 April 1
# 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A.

CHANDRA X-RAY OBSERVATIONS OF NGC 1316 (FORNAX A) Dong-Woo Kim and G. Fabbiano
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 Received 2002 June 25; accepted 2002 December 9

ABSTRACT We report the results of the Chandra ACIS subarcsecond resolution X-ray observation of the archetypal merger radio galaxy NGC 1316 (Fornax A). We confirm the presence of fine substructures in the hot interstellar medium (ISM). Some of these are likely to result from interaction with the radio jets, while others may be related to a complex intermingling of different phases of the ISM. We detect a low-luminosity X-ray active galactic nucleus (AGN) with LX ¼ 5 á 1039 ergs sþ1 (in 0.3­8 keV) and a þ ¼ 1:7 power-law energy spectrum. We also detect 81 point sources within the 25th magnitude isophotal ellipse of NGC 1316 (LX in the range of 2 á 1037 to 2 á 1039 ergs sþ1), with hard (kT $ 5 keV) X-ray spectra, typical of X-ray binaries, and a spatial radial distribution consistent with that of the optical (i.e., stellar) surface brightness. We derive the X-ray luminosity function (XLF) of these sources, correcting for the incompleteness at the faint end caused by the presence of the diffuse emission from the hot ISM in the central regions of NGC 1316 and by the widening of the Chandra point-spread functions at increasing distance from the aim point. With these corrections, the XLF is well reproduced by a single--unbroken--power law with a slope of þ1.3 down to our threshold luminosity of $3 á 1037 ergs sþ1. The hot ISM has temperatures in the 0.5­0.6 keV range, its surface brightness distribution is more centrally concentrated than that of the point sources, and its temperature appears to decrease at larger radii. These properties suggest that the ISM may be subject to partial winds. Taking into account the spectral complexity of the ISM, and the presence of unresolved low luminosity X-ray sources (which can be inferred from the spectra), we constrain the metal abundance of the hot ISM to be Z ¼ 0:25­ 1.3 Z (90% confidence). Subject headings: galaxies: abundances -- galaxies: individual (NGC 1316, NGC 1317) -- galaxies: ISM -- X-rays: galaxies

1. INTRODUCTION

The radio galaxy NGC 1316 (Fornax A) is a disturbed elliptical galaxy with numerous tidal tails. To explain this morphology, Schweizer (1980) suggested several low-mass, gas-rich mergers occurring over the last 2 Gyr (see also Ekers et al. 1983; Kim, Fabbiano, & Mackie 1998, hereafter KFM; Mackie & Fabbiano 1998). NGC 1316 has been extensively observed in a wide range of wavelengths (see a summary of previous observations in KFM). In the radio band, Fornax A is the third brightest object in the sky, with giant radio lobes (Wade 1961; Ekers et al. 1983), separated by $200 kpc, consisting of polarized filaments (Fomalont et al. 1989) and S-shaped nuclear radio jets (Geldzahler & Fomalont 1984). In X-rays, it was observed with Einstein (Fabbiano, Kim, & Trinchieri 1992), ROSAT PSPC (Feigelson et al. 1995), ASCA (Kaneda et al. 1995; Iyomoto et al. 1998), and ROSAT HRI (KFM). In particular, the ROSAT observations revealed $109 M of hot ISM, with an inhomogeneous distribution. The substructures of the ISM were not highly significant, given the ROSAT HRI data quality, but nevertheless suggested a multiphase ISM interacting with the radio jets (KFM). NGC 1316 is the first elliptical galaxy for which this type of jet/hot ISM interaction has been reported. Previous evidence of this phenomenon had been limited to galaxy clusters (Cygnus A, Carilli, Perley, & Harris 1994; the Perseus cluster, Bohringer et al. 1993). Chandra observations are now revealing many other examples in several other elliptical galaxies and clusters (e.g., NGC 4374, Finoguenov & Jones 2001; and Hydra A, McNamara et al. 2000). 826

In this paper we report the results of a high spatial resolution, spectrally resolved Chandra ACIS (Weisskopf et al. 2000) observations of NGC 1316. The motivation of this work is twofold. First, we attempt to confirm and study in detail the features of the hot ISM suggested by the ROSAT HRI (KFM). Second, NGC 1316 is an X-ray­faint elliptical (Fabbiano et al. 1992), where we would expect a large contribution to the X-ray emission to originate from low-mass X-ray binaries (LMXBs; e.g., Trinchieri & Fabbiano 1985; Canizares, Fabbiano, & Trinchieri 1987; Kim, Fabbiano, & Trinchieri 1992; Eskridge, Fabbiano, & Kim 1995a, 1995b; Fabbiano, Kim, & Trinchieri 1994b; Pellegrini & Fabbiano 1994). With Chandra we can detect individual LMXBs (e.g., Sarazin, Irwin, & Bregman 2000), study their properties, and quantitatively estimate their contribution to the diffuse emission. We can also significantly reduce the bias introduced by the presence of unresolved sources in past discussions of the spectral and spatial characteristics of the ISM. This paper is organized as follows. In x 2, we describe the Chandra observations, the data reduction, and the results of spatial and spectral analyses. In x 3, we derive the X-ray luminosity function (XLF) of point sources associated with NGC 1316 and estimate the uncertainties derived from the varying detection thresholds across the field. In x 4, we summarize various emission components. In x 5, we discuss the implications of our results for the nature and properties of the hot ISM and its interaction with radio jets and other phases of ISM. Finally, we summarize our conclusions in x 6. We adopt a distance D ¼ 18:6 Mpc throughout this paper, based on the Hubble Space Telescope (HST ) measurements of Cepheid variables (Madore et al. 1999)


CHANDRA X-RAY OBSERVATIONS OF NGC 1316 in NGC 1365. At the adopted distance, 100 corresponds to 90 pc.
2. CHANDRA OBSERVATIONS AND DATA ANALYSIS

827

NGC 1316 was observed for 30 ks on 2001 April 17 (ObsID 2022), with the Chandra Advanced CCD Imaging Spectrometer (ACIS; Garmire 1997). We used the backilluminated CCD S3 (CCD ID 7) because of its sensitivity at low energies. To include NGC 1317 (6<3 away from NGC 1316) in the same S3 chip, a small offset was applied to the SIM (Science Instrument Module) position. NGC 1316 was kept close to on-axis to achieve the best spatial resolution. The data were reduced with XPIPE (Kim et al. 2003), a custom pipeline specifically developed for the Chandra Multiwavelength Project (ChaMP). XPIPE takes the CXC pipeline level 2 data products and then applies additional data corrections (e.g., gain correction, removing bad pixels/ columns) and additional data screening (e.g., removing background flares), performs source detection, and determines source properties, such as flux, X-ray colors, variability, and extent. Specifically, for this observation, we have identified two bad pixels in CCD S2 (or CCD ID 6), which resulted in five spurious sources. The CXC pipeline processing was done before the new S3 gain file was released in 2001 September. We have rerun acis_process_events to correct the ACIS gain and used follow-up tools available in CIAO1 to generate CXC pipeline­like products. Background flares are often seen in back-illuminated (BI) chips (CCD S1 and S3). They are excluded when the background rate is beyond 3 from the average rate, which is measured iteratively after initial exclusion of flares. Removal of background flares reduced the effective exposure time of CCD S3 to 24.7 ks. To detect X-ray sources, we used WAVDETECT (Freeman & Vinay 2002), a wavelet detection algorithm available in CIAO. WAVDETECT is more reliable in finding individual sources (and not detecting false sources) in a crowded field containing extended emission than the traditional sliding-box CELLDETECT algorithm, although it requires a longer processing time. We set the WAVDETECT significance threshold parameter to be 10þ6, which corresponds to 1 possibly spurious source, and the scale parameter to cover seven steps between 1 and 64 pixels. This made us sensitive to sources ranging from pointlike to 3200 in size, and in particular accommodates the variation of the point-spread function (PSF) as a function of the off-axis angle. WAVDETECT tends to detect spurious sources near the detector edge. To avoid such false detections, we have utilized an exposure map (made at 1.5 keV) and applied a 10% exposure threshold. The exposure map was tailored to each CCD, based on the aspect history. To extract source properties (such as count rates, spectra, etc.), we have used the 95% encircled energy (at 1.5 keV) radius centered at the WAVDETECT centroid, with a minimum of 300 to accommodate the radial variation of PSF. Background counts were determined locally for each source from an annulus from 2 to 5 times the source radius, after excluding nearby sources. 2.1. Point Sources The detected X-ray sources are shown in Figure 1 superimposed on the X-ray (left panel ) and on the Digitized Sky
1

Survey2 optical (right panel ) images. In this figure (and throughout this paper), north is to the top and east is to the left in the image. Extended sources are found at the locations of NGC 1316 and NGC 1317 as seen in ROSAT data (KFM). In addition, the Chandra observations reveal 94 sources, 83 of them in CCD S3. Of these, 81 sources (77 in S3 and 4 in S2) are within the D25 ellipse (taken from de Vaucouleurs et al. 1991 [RC3]) of NGC 1316. The source density increases toward the center of NGC 1316, indicating that most of them are related to NGC 1316. Three sources are found within D25 of NGC 1317, with the brightest, extended one at the center of NGC 1317. The list of sources (including sources found in other CCDs) is given in Table 1. The net source counts estimated by XPIPE (i.e., by aperture photometry as described above) are usually in good agreement with those determined by WAVDETECT. Exceptions are those sources within 2000 from the center of NGC 1316, where the extended diffuse X-ray emission makes it difficult to accurately measure source and background counts. Consequently, the net counts and rates are subject to a large uncertainty, and these sources are marked in the table (they are not used below in determining XLF and in spectral fitting). Also marked in the table are those sources that have one or more sources within their source extraction radius, introducing additional uncertainty in their count rates. Three sources are found at the edge of the chip, and their counts should be considered as a lower limit. These are marked in Table 1. After correcting for effective exposure and vignetting, the X-ray flux in the 0.3­8.0 keV band is calculated with an energy conversion factor (ECF) assuming a powerlaw source spectrum with þph ¼ 1:7 and NH ¼ 3 á 1020 cmþ2; ECF ¼ 6:037 á 10þ12 ergs cmþ2 sþ1 per 1 count sþ1 for the back-illuminated (BI) chips and 9:767 á 10þ12 ergs cmþ2 sþ1 for the front-illuminated (FI) CCD chips. With the adopted distance of 18.6 Mpc, the X-ray luminosities of the point sources range from $2 á 1037 to $8 á 1039 ergs sþ1. We have identified one possible off-center ultraluminous X-ray source (ULX) with LX ¼ 2:4 á 1039 ergs sþ1 (CXOU J032251.2þ370949). Following Zezas & Fabbiano (2002), we define the ULX as a non-AGN (i.e., off-center) point source with LX > 2 á 1039 ergs sþ1. This source is marked in Figure 1 and also in Table 1. No optical counterpart is seen in the DSS image (see Fig. 1). There are three more sources with net count above 200 (or, LX > a few á 1039 ergs sþ1) within the D25 ellipse of NGC 1316 (see Table 1). Two of them correspond to the elongated feature at the center of NGC 1316 (see x 2.2). The third source, CXOU J032241.2þ371235, is 1000 SW from the center; hence its X-ray flux is highly uncertain because of the strong diffuse X-ray emission. Counting pixel values manually suggests that its count might be overestimated by as much as $50%. Five sources are found to be coincident with globular clusters identified in HST images (Shaya et al. 1996) and in ground observations (Goudfrooij et al. 2001). They are marked as such in Table 1. Also identified is one potential super­soft X-ray source (SSS), CXOU J032235.9þ371135, for which all X-ray photons are in the soft band (0.3­0.9 keV). Based on the log N log S of Chandra Deep Field sources (Brandt et al. 2001; Giacconi et al. 2001) and ChaMP sources (Kim et al. 2003), we expect fewer than seven
2

See http://cxc.harvard.edu/ciao.

See http://stdatu.stsci.edu/dss.


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Fig. 1.--X-ray sources superimposed on the X-ray (left) and on the Digitized Sky Survey optical (right) images. NGC 1316 is at the center of the DSS image, and NGC 1317 is to the north of NGC 1316. The horizontal bar in the lower left corner indicates 10 . The circle radius indicates the PSF size, while the circle color indicates WAVDETECT source significance (red,>5 ; blue, 3­5 ; green, <3 ). The source marked with a square is a possible ULX source. North is to the top and east is to the left.

serendipitous sources within D25 of NGC 1316 in S3. The radial distribution of point sources is also consistent with the radial profile of the optical light, i.e., the stellar distribution (see x 2.3), suggesting that most of them are LMXBs associated with NGC 1316. The spectral properties of these sources are also consistent with this hypothesis (x 2.4.1). 2.2. Surface Brightness Distribution of the Diffuse X-Ray Emission To identify the substructures of extended, diffuse X-ray emission, we have applied CSMOOTH, an adaptive smoothing algorithm available in CIAO. Figure 2 shows the smoothed image within the central 30 á 30 region. In this arcminute-scale image, the diffuse X-ray emission is elongated in the north-south direction, and does not follow either the major axis (P:A: ¼ 50 ) or the minor axis of NGC 1316. The ellipse in the center of Figure 2 indicates the optical figure of NGC 1316 with size equal to 1/10 of D25. Also noticeable is a secondary maximum of the surface brightness (`` blob '') at 3000 ­6000 north of the center. This feature is extended when compared to the PSF, and its X-ray emission is possibly soft (see x 2.4.3). We address the nature of these large-scale north-south elongations in x 5. In the subarcminute scale, the X-ray surface brightness is elongated along the major axis of the optical figure, but it is far from featureless. The enlarged view of the central region of NGC 1316 is shown in Figure 3. It is clearly noticeable that the X-ray surface brightness distribution forms valleys

(cavities) toward the southeast (P:A: ¼ 120 ) and northwest (P:A: ¼ 315 ). These are the directions along which the radio jets propagate (see Fig. 2 in Geldzahler & Fomalont 1984). In Figure 3, red lines indicate the directions and approximate sizes of the radio jets (see x 5.2 for further discussions of the interaction between the hot ISM and radio jets). It was one of the main purposes of this observation to confirm the reality of these X-ray valleys, which were suggested by the ROSAT HRI image (KFM). If we compare the counts within a 300 radius circle in the X-ray valley and in the surrounding region at a similar distance from the center, the difference is significant at a $10 level. The central 300 region exhibits a double-peak feature, elongated toward the northeast (see also Fig. 4). Figure 4 shows the central 30 á 30 smoothed X-ray images in different energy bands: soft (0.3­0.9 keV), medium (0.9­ 2.5 keV), and hard (2.5­8.0 keV). The diffuse emission is most prominent in the soft band, as expected from the hot gaseous X-ray emission. The northern blob is also most clearly seen in the soft band (see below for more discussion). The point sources, on the other hand, are seen more distinctly in the medium band, as expected for LMXBs with a harder spectrum. A point source at the nucleus is unambiguously identified in the hard band. The location of the nucleus determined from this hard-band image is marked as a circle at the center of Figure 3. A true-color image made by combining the three band images (red for the soft band, green for the medium band, and blue for the hard band) is shown in Figure 5.


TABLE 1 Source List Source Radius (arcsec)

Source

CCD No.

Detect No.

R.A. (J2000)

Decl. (J2000)

Net Counts

Error

Counts ksþ1

LXa (1038 ergs sþ1)

Notesb

Within the D25 Ellipse of NGC 1316 CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU J032219.5þ371338 J032219.9þ371322 J032228.9þ371443 J032229.5þ371511 J032225.6þ371145 J032227.5þ371223 J032228.9þ371242 J032229.1þ371023 J032230.4þ371025 J032232.6þ371309 J032235.2þ371127 J032235.2þ371205 J032235.3þ371248 J032235.5þ371313 J032235.6þ371248 J032235.7þ371218 J032235.9þ371135 J032235.9þ371256 J032236.4þ370842 J032236.4þ371324 J032236.6þ371054 J032236.6þ371306 J032237.2þ371212 J032237.4þ371301 J032237.5þ371428 J032237.6þ371252 J032238.7þ371221 J032238.7þ371422 J032239.1þ371148 J032239.3þ371313 J032239.4þ371252 J032239.4þ371256 J032239.6þ371243 J032239.9þ371056 J032240.1þ371310 J032240.4þ371244 J032240.5þ371227 J032240.7þ371151 J032240.8þ371224 J032241.1þ371235 J032241.3þ371117 J032241.7þ371229 J032241.7þ371343 J032241.8þ371207 J032241.8þ371225 J032241.9þ371238 J032241.9þ371305 J032242.0þ371218 J032242.0þ371246 J032242.0þ371256 J032242.1þ371123 J032242.3þ371260 J032242.5þ371222 J032242.5þ371258 J032242.7þ371217 J032242.8þ371222 J032243.2þ371206 J032243.3þ371104 J032243.7þ371215 J032243.8þ371233 J032243.9þ371203 ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... ........... 6 6 6 6 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 6 5 1 4 83 78 63 62 61 60 26 59 25 24 58 57 23 56 82 22 55 54 21 53 52 51 50 20 19 18 49 48 76 47 17 46 16 15 14 13 45 12 11 10 44 43 42 9 41 8 7 6 5 40 4 39 38 3 75 2 37 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 19.5 19.9 28.9 29.5 25.6 27.5 28.9 29.1 30.4 32.6 35.2 35.2 35.3 35.5 35.6 35.7 35.9 35.9 36.4 36.4 36.6 36.6 37.2 37.4 37.5 37.6 38.7 38.7 39.1 39.3 39.4 39.4 39.6 39.9 40.1 40.4 40.5 40.7 40.8 41.1 41.3 41.7 41.7 41.8 41.8 41.9 41.9 42.0 42.0 42.0 42.1 42.3 42.5 42.5 42.7 42.8 43.2 43.3 43.7 43.8 43.9 þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 13 13 14 15 11 12 12 10 10 13 11 12 12 13 12 12 11 12 08 13 10 13 12 13 14 12 12 14 11 13 12 12 12 10 13 12 12 11 12 12 11 12 13 12 12 12 13 12 12 12 11 12 12 12 12 12 12 11 12 12 12 37.6 21.8 42.7 11.3 45.2 23.3 41.6 23.1 25.1 09.4 26.8 05.3 47.5 13.2 47.6 18.1 34.9 56.1 42.0 23.7 54.5 06.0 11.6 00.9 28.2 51.5 20.9 21.5 48.4 12.8 52.5 56.0 43.0 55.9 10.2 44.5 26.7 51.4 23.9 35.4 17.4 29.0 43.2 07.4 25.1 38.1 04.9 18.5 45.5 56.1 23.3 59.5 21.5 57.5 17.1 22.2 06.3 03.8 15.0 32.7 02.7 3.44 3.22 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 5.24 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 11.32 6.34 3.87 8.69 8.75 7.87 22.48 4.92 7.26 5.72 32.78 10.90 26.80 75.54 23.96 11.10 12.04 8.67 11.89 72.40 3.77 17.24 7.53 7.76 7.18 20.72 4.66 31.72 23.71 19.95 8.68 10.75 22.06 22.02 1.48 31.87 32.08 28.12 54.97 248.57 28.52 805.64 3.95 14.45 440.46 52.86 11.35 5.46 10.00 19.77 65.08 42.73 56.18 18.42 6.69 29.86 3.03 36.39 25.81 21.89 8.33 4.72 3.97 3.41 4.29 4.44 4.29 6.09 3.80 4.30 3.98 7.16 4.99 6.56 9.94 6.28 5.12 5.12 4.60 5.48 9.77 3.81 5.57 4.88 4.60 4.14 6.20 4.61 6.91 7.02 6.40 5.50 5.72 7.12 6.29 4.64 9.22 10.57 7.82 11.86 19.24 7.26 31.17 4.47 6.61 24.47 13.06 6.04 9.88 8.96 7.13 9.61 8.44 11.76 6.50 9.06 10.43 4.91 7.48 7.84 7.92 5.14 0.40 0.22 0.15 0.32 0.36 0.32 0.93 0.22 0.32 0.23 1.37 0.46 1.09 3.06 0.97 0.47 0.51 0.35 0.59 2.94 0.15 0.70 0.31 0.33 0.29 0.89 0.19 1.29 1.00 0.85 0.35 0.44 0.92 0.91 0.06 1.32 1.34 1.18 2.30 10.39 1.18 33.70 0.16 0.60 18.40 2.20 0.47 0.23 0.41 0.82 2.69 1.77 2.34 0.76 0.27 1.23 0.12 1.55 1.07 0.90 0.34 1.62 0.89 0.61 1.29 0.90 0.81 2.31 0.55 0.81 0.57 3.43 1.16 2.72 7.66 2.42 1.18 1.27 0.86 1.47 7.35 0.39 1.74 0.77 0.83 0.73 2.22 0.48 3.23 2.50 2.13 0.88 1.10 2.30 2.28 0.15 3.31 3.34 2.94 5.75 25.97 2.94 84.21 0.40 1.51 45.98 5.51 1.18 0.57 1.03 2.04 6.72 4.43 5.84 1.89 0.68 3.09 0.31 3.87 2.66 2.26 0.84

2 2 9

5

2 2 5

1, 2 1, 2 1, 7 1, 2, 6

1, 6 1, 5 1, 5 1 2 2 1, 2 2 1, 2, 5 1, 2


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KIM & FABBIANO
TABLE 1--Continued Source Radius (arcsec) 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 3.00 4.10 8.18 3.21 5.43 3.68 4.03 5.54 6.48 9.57

Vol. 586

Source CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU J032244.2þ371053 ........... J032244.8þ371210 ........... J032245.2þ371423 ........... J032245.4þ371226 ........... J032245.4þ371306 ........... J032245.6þ371207 ........... J032245.8þ371214 ........... J032247.1þ371408 ........... J032247.5þ371240 ........... J032248.3þ371159 ........... J032249.3þ371152 ........... J032249.4þ371033 ........... J032250.9þ370813 ........... J032251.0þ371206 ........... J032251.2þ370949 ........... J032252.2þ371158 ........... J032253.6þ371211 ........... J032254.3þ371027 ........... J032259.7þ371128 ........... J0323 5.7þ371113 ............

CCD No. 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7

Detect No. 36 35 73 34 72 33 1 71 70 32 31 30 79 69 29 28 27 68 66 65

R.A. (J2000) 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 22 23 44.2 44.8 45.2 45.4 45.4 45.6 45.8 47.1 47.5 48.3 49.3 49.4 50.9 51.0 51.2 52.2 53.6 54.3 59.7 05.7 þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ þ

Decl. (J2000) 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 37 10 12 14 12 13 12 12 14 12 11 11 10 08 12 09 11 12 10 11 11 53.2 09.7 22.7 25.5 06.2 06.7 13.8 07.5 39.7 58.9 52.0 33.0 13.3 05.8 49.2 57.9 11.1 26.8 27.7 13.0

Net Counts 9.48 11.36 8.78 2.00 12.63 8.11 19.58 4.25 9.46 6.68 16.62 5.23 17.98 10.68 227.86 14.45 15.28 14.82 26.05 92.49

Error 4.87 5.60 4.29 4.17 5.24 5.01 6.21 3.62 4.73 4.30 5.46 4.75 7.54 4.86 16.54 5.47 5.58 5.91 7.35 11.82

Counts ksþ1 0.41 0.46 0.52 0.08 0.51 0.33 0.80 0.23 0.38 0.27 0.68 0.21 0.78 0.43 9.46 0.59 0.62 0.65 1.09 3.96

LXa (1038 ergs sþ1) 1.03 1.16 1.30 0.20 1.29 0.83 2.00 0.57 0.95 0.68 1.71 0.51 1.95 1.08 23.65 1.47 1.56 1.62 2.72 9.90

Notesb

3

3

4

Within the D25 Ellipse of NGC 1317 CXOU J032240.7þ370518 ........... CXOU J032244.3þ370614 ........... CXOU J032246.1þ370552 ........... 7 7 7 81 74 80 3 22 40.7 3 22 44.3 3 22 46.1 þ 37 05 18.4 þ 37 06 14.0 þ 37 05 51.9 15.26 11.79 13.79 1.03 366.52 47.13 9.23 21.45 11.82 0.07 16.39 2.16 0.17 40.97 5.40 3 8

Beyond D25 of NGC 1316 and NGC 1317 CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU CXOU J032145.8þ370430 ........... J032147.1þ370723 ........... J032159.4þ370515 ........... J032137.5þ371454 ........... J0322 0.7þ371918 ............ J032211.1þ370954 ........... J032212.6þ371212 ........... J032215.4þ371656 ........... J032225.7þ370912 ........... J032230.8þ370736 ........... J032254.7þ370706 ........... 2 2 2 5 6 6 6 6 7 7 7 3 2 1 1 16 12 11 7 64 77 67 3 3 3 3 3 3 3 3 3 3 3 21 21 21 21 22 22 22 22 22 22 22 45.8 47.1 59.4 37.5 00.7 11.1 12.6 15.4 25.7 30.8 54.7 þ þ þ þ þ þ þ þ þ þ þ 37 37 37 37 37 37 37 37 37 37 37 04 07 05 14 19 09 12 16 09 07 07 29.9 23.4 15.3 53.7 18.2 53.8 11.8 55.9 12.0 36.1 06.5 40.00 31.57 28.50 34.29 22.29 8.56 5.84 8.03 5.22 7.77 11.84 113.70 87.04 180.51 384.08 197.23 30.20 26.37 78.53 136.60 49.72 74.48 19.81 16.67 18.68 32.73 17.55 7.66 6.75 10.45 13.09 9.28 11.84 4.447 3.177 6.489 17.639 8.064 1.111 0.958 3.034 6.268 2.234 3.461

a L (in 0.3­8.0 keV) is determined with D ¼ 18:6 Mpc and ECF ¼ 6:037 (or 9:767÷á 10þ15 ergs sþ1 for 1 count ksþ1, which is appropriate in BI (or FI) X CCDs for a source with photon index 1.7 and N ÏH÷ ¼ 3 á 1020 cmþ2. b Notes: (1) Sources within 2000 from the center of NGC 1316. The source count may be contaminated by the diffuse emission. (2) There is another source(s) within the source extraction radius. (3) Sources fall near the edge of the detector. The source count should be considered as a lower limit. (4) A potential ULX source. (5) Coincident with globular clusters listed in Shaya et al. 1996 and Goudfooij et al. 2001. (6) At the center of NGC 1316. (7) Closeto the center of NGC 1316. Its count may be overestimated. (8) At the center of NGC 1317. (9) A potential super soft X-ray source.

2.3. Radial Profiles of Diffuse X-Ray Emission and Point Sources We have derived radial surface brightness profiles to study the radial distribution of the hot gas and point-source components and compare them with the optical (stellar) distribution. Given the obvious lack of circular symmetry of the diffuse X-ray emission, we have extracted radial profiles from different angular sectors, after excluding detected point sources. Beta models, ôx $ ½1 ×Ïr=a÷2 þ3×0:5 , were then used to model these profiles. Toward the east-west direction at P:A: ¼ 30 ­150 and 210 ­330 , excluding the northern blob and the less prominent southern extension, the radial profile is smooth and the best-fit  is 0.57­0.59 at 90% confidence, corresponding to a radial slope of þ2.4 to þ2.5. Toward the north-south direc-

tion, however, the radial profile steepens around 2000 ­3000 and then flattens because of the elongated features. The best-fit  is 0.43­0.49 at 90% confidence, which corresponds to a radial slope of þ1.6 to þ1.9. The X-ray radial profile measured toward the east-west direction is shown in Figure 6, where observed data points are marked by open circles with error bars and the best-fit beta model is represented by the dashed line. Although the data are well fitted in most radial bins, there is a significant deviation from the beta model at the nucleus, which requires an additional point source. This nuclear source is most prominent in the hard-band X-ray image (Fig. 4). We have used a CIAO tool mkpsf to reproduce a point source at the center. The intensity of this nuclear source is consistent with the results of the X-ray spectral fitting (see x 2.4.2). The solid line in Figure 6 indicates the composite beta model+central point source


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Fig. 2.--Chandra X-ray image of the central 30 á 30 region of NGC 1316. The data were adaptively smoothed. The ellipse indicates the optical figure of NGC 1316, with size equal to 1/10 of D25 taken from RC3. The horizontal bar in the lower left corner is 3000 long. North is to the top and east is to the left.

profile. The central source profile is marked by the dotted line in the same figure. The estimated X-ray flux of the nuclear component is 1:2 á 10þ13 ergs sþ1 (with a 15% error) in the broad energy band (0.3­8 keV). Also plotted in the Figure 6 (green) is the radial profile of the stellar light distribution from the HST I band (Shaya et al. 1996). The I-band profile decreases radially as rþ1:16 and is much flatter than the radial distribution of the diffuse X-ray emission. The X-ray point sources detected in the Chandra observations (Fig. 6, red squares) are distributed like the stellar light, as would be expected from LMXBs in NGC 1316, instead of following the diffuse X-ray emission. This means that the contribution from LMXBs to the X-ray emission becomes more significant at the outer radii. This has an important implication when considering the effect of hidden populations of LMXBs in X-ray­faint early-type galaxies observed with lower angular resolution than Chandra. In particular, lower resolution data would give a biased distribution of the hot ISM, and wrong (in excess) mass measurements, if the contribution of LMXBs is ignored. Ignoring the LMXBs would also affect spectral results (see x 5 for further discussion).

2.4. Spectral Analysis Following the science threads,3 we have produced response files (rmf and arf ) to be used in the spectral fitting. We have also applied a new method to produce weighted response files to take into account the variation with detector location,4 but the results are almost the same. After this paper was submitted, a time-dependent degradation of the low-energy ACIS quantum efficiency was reported.5 We have regenerated the spectral response files and rerun all the spectral fitting. We found that the spectral parameter most affected is NH, which can become lower by as much as a factor of 2. The kT of the softer spectral component in multicomponent fits also becomes slightly lower. However, the main results remain the same. We report here the results from the latest analysis, performed with the best available calibration.
See http://cxc.harvard.edu/ciao/documents_threads.html. As described in the science thread available at http://cxc.harvard.edu/ ciao. 5 See http://cxc.harvard.edu/cal/Links/Acis/acis/Cal_prods/qeDeg/ index.html.
4 3


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Fig. 3.--Enlarged view of the central region of NGC 1316 from the Chandra X-ray data (adaptive smoothing applied). The horizontal bar in the lower left corner is 1000 long. The location of the nucleus determined in the hard-band image is marked by a green circle. A few contours are drawn to illustrate the X-ray valleys along P:A: $ 120 and $315 where the radio jets (red lines) are propagating. North is to the top and east is to the left.

The background spectrum was extracted from five circular, source-free regions with a 6000 radius in CCD S3, situated between 20 and 50 from the center of NGC 1316. Different choices of background regions within the same CCD do not change our results, because point sources (the nucleus and LMXBs) are well within very small source regions and the diffuse emission is extended only to $10 ­20 . We have fitted, within an energy range of 0.3­5.0 keV, emission models including a thermal gas model (MEKAL), bremsstrahlung, and power-law, alone and in combination. For solar abundances, we take the photospheric values given in Anders & Grevesse (1989), which is about 40% larger than the meteoric value in Fe. The spectral fitting results are summarized in Tables 2­5. We discuss these results below, for the different galactic components.
2.4.1. Point Sources

point sources only at galactocentric radii r > 2000 to avoid confusion with the strong diffuse emission near the center of NGC 1316. We have only used sources found in CCD S3, to avoid the complexity introduced by different detector responses. We find that the observed spectra of point
TABLE 2 Spectral Fitting of the Combined Point Source Spectrum NH (1022 cmþ2) 0.000 (0.01) 0.000 (0.01) 0.054 (0.02) 0.025

Modela 1 2 3 4 ............. ............. ............. .............

kT/Cph 5.57 3.29 2.03 1.85 (1.5) (1.0) (0.1) (0.1)

Z 1.00



2 reduced

(2/dof)

0.97 0.74 0.74 0.69

(=76.7/79) (=58.1/79) (=58.1/79) (=55.2/80)

Since most point sources are not bright enough for individual spectral analysis, we have co-added their spectra to determine their average spectral properties. We have used

Note.--Errors in parentheses are at the 90% confidence level for one interesting parameter. a Total counts = 1730. Model 1: one-component model; MEKAL, abundance fixed to solar. Model 2: one-component model; bremsstrahlung. Model 3: one-component model; power law. Model 4: onecomponent model; power law with fixed NH.


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Fig. 4.--Adaptively smoothed images of the central 30 á 30 region of NGC 1316 in different energy bands: (a) the soft band in 0.3­0.9 keV, (b) the medium band in 0.9­2.5 keV, and (c) the hard band in 2.5­8.0 keV. North is to the top and east is to the left.

sources are well fitted with single-component models, either a thermal model with best-fit temperature of kT $ 4­6 keV or a power-law model with best-fit photon index of þph $ 2:0 (Table 2). This power-law spectrum is softer than those determined in a few other early-type galaxies (e.g., NGC 4697; Sarazin et al. 2001: þph $ 1:6). However, if NH is fixed at the Galactic value, a softer þph $ 1:8 is obtained, more in keeping--within the errors--with these other studies. The spread of X-ray colors of point sources is well within the range of those found in other galaxies (see below). More conservatively, we have also used sources only at r > 6000 , where the diffuse emission reaches the background

level. The results are almost the same. Excluding the brightest source (the ULX candidate, CXOU J032251.2þ370949), to confirm that the average properties are not dominated by a small number of peculiar sources, does not affect the results. We have also investigated the spectral properties of the sources by means of X-ray colors. In Figure 7, we plot individual point sources detected with more than 20 counts in an X-ray color-color diagram. Following the ChaMP convention, (also similar to those previously used in studying Einstein data by Kim et al. 1992), we have defined two X-ray colors to represent two spectral parameters, absorption

Fig. 5.--True color image of the central 40 á 40 region of NGC 1316 with red for the soft band in 0.3­0.9 keV, green for the medium band in 0.9­2.5 keV, and blue for the hard band in 2.5­8.0 keV. North is to the top and east is to the left.


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Fig. 6.--Radial profile of the diffuse X-ray emission (open circles) and point sources (red squares). The solid and dashed lines indicate the beta-model predictions with and without AGN (dotted line) at the center. For comparison, the I-band radial profile is also plotted in green. The y-axis zero points of the I-band and point-source distributions were rescaled to make the two distributions fit in a single plot. This does not change the radial dependence of the profiles.

and slope: C21 ¼ þ logÏcounts in 0:9 2:5 keV÷ × logÏcounts in 0:3 0:9 keV÷ ; C32 ¼ þ logÏcounts in 2:5 8:0 keV÷ × logÏcounts in 0:9 2:5 keV÷ : There are several reasons for this particular selection of energy bands (see Kim et al. 2003 for details). In particular, we want to (1) isolate the two spectral parameters (i.e., C21 is mostly sensitive to the absorption and C32 to the spectral

slope) and (2) distribute the spectral counts almost equally in the three energy bands for a typical source with þph $ 2:0, so that we can achieve the highest possible statistical significance. In Figure 7, filled circles are for source with more than 50 counts, open circles for sources with counts between 30 and 50, and stars (without corresponding error bars) for sources with counts between 20 and 30. The grid indicates the predicted locations of sources with various photon indices (from 0 to 4) and absorption column densities (from 1020 to 1022 cmþ2). The points are scattered in the X-ray color-color diagram to the extents comparable to errors in X-ray colors, with a centroid of their distribution

TABLE 3 Spectral Fitting of Diffuse X-Ray Emission: Central Bin (r < 500 ; Total Counts = 1613) F Modela 1 .............. 2 .............. 3 .............. NH (1022 cmþ2) 0.00 (0.01) 0.11 (0.01) 0.02 (0.01) kT1 0.65 (0.03) 0.61 (0.03) 0.62 (0.03) Z 1.00 0.13 (0.01) 1.00 Cph Total 1.84 2.05 2.71
b X

Component 1

Component 2

2 2 reduced ( /dof)

1.76 (0.2)

1.43

1.28

2.06(= 125.8/61) 1.13(= 67.7/60) 0.64(= 38.0/59)

Note.--Errors in parentheses are at the 90% confidence level for one interesting parameter. a Model 1: one-component model; MEKAL with fixed Z. Model 2: one-component model; MEKAL with varying Z. Model 3: twocomponent model; MEKAL + power law. b F is in units of 10þ13 ergs sþ1 cmþ2 in a 0.3­8.0 keV energy band. X


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CHANDRA X-RAY OBSERVATIONS OF NGC 1316
TABLE 4 Spectral Fitting of Diffuse X-Ray Emission: Outskirts (r ¼ 500 ­6000 ) NH (1022 cmþ2) FX kT1 Z kT2/Cph Total
b

835

Modela

Component 1

Component 2



2 reduced

(2/dof)

(r ¼ 500 ­1500 ; Total Counts = 1851) 1 2 3 4 .............. .............. .............. .............. 0.00 0.05 0.00 0.05 (0.01) (0.02) (0.01) (0.01) 0.65 0.63 0.64 0.63 (0.02) (0.04) (0.03) (0.03) 1.00 0.21 (0.04) 1.00 1.00 2.21 2.40 2.52 2.55 1.37 0.71 0.70 0.64 (=79.5/58) (=40.7/57) (=39.0/56) (=36.0/56)

1.38 (1.5) 2.74 (0.6)

1.82 1.75

0.70 0.81

(r ¼ 1500 ­3000 ; Total Counts = 1168) 1 2 3 4 .............. .............. .............. .............. 0.00 0.00 0.00 0.00 (0.01) (0.01) (0.01) (0.01) 0.54 0.59 0.60 0.59 (0.03) (0.03) (0.04) (0.04) 1.00 0.26 (0.02) 1.00 1.00 1.08 1.23 1.23 1.27 1.37 1.03 1.05 1.06 (=64.2/47) (=47.6/46) (=47.0/45) (=47.5/45)

0.45 (c) 2.98 (0.8)

0.93 0.95

0.29 0.31

(r ¼ 3000 ­6000 ; Total Counts = 2520) 1 2 3 4 .............. .............. .............. .............. 0.00 0.00 0.00 0.00 (0.01) (0.01) (0.01) (0.01) 0.42 0.50 0.52 0.51 (0.04) (0.04) (0.04) (0.04) 1.00 0.22 (0.03) 1.00 1.00 1.85 2.11 2.12 2.16 1.07 0.81 0.80 0.81 (=83.5/78) (=62.5/77) (=60.5/76) (=61.7/76)

0.32 (c) 3.60 (1.0)

1.60 1.64

0.52 0.52

Note.--Errors in parentheses are at the 90% confidence level for one interesting parameter. a Model 1: one-component model; MEKAL with fixed Z. Model 2: one-component model; MEKAL with varying Z. Model 3: twocomponent model; MEKAL + power law. Model 4: two-component model; MEKAL + bremsstrahlung. b F is in units of 10þ13 ergs sþ1 cmþ2 in a 0.3­8.0 keV energy band. X c Not constrained.

around þph $ 2:0 and NH $ a few á 1020 cmþ2. This is consistent with the average properties obtained by fitting the combined spectra. The filled circle surrounded by a larger open circle in Figure 7 indicates the brightest source, CXOU J032251.2þ370949, the ULX. Its spectrum appears to be slightly absorbed (NH $ a few á 1021 cmþ2) and steep (þph $ 2:5­4.0). Both spectral parameters are within the range of the ULXs found in the Antennae galaxies (Zezas et al. 2002; see Fig. 13 in their paper). If we assume þph ¼ 3:5 and NH ¼ 2 á 1021 cmþ2, then its luminosity increases by a factor of 2, i.e., LX ¼ 4:7 á 1039 ergs sþ1. We do not see temporal variability of this source either by binning the data or by applying a Bayesian-block analysis to the unbinned data (developed by J. Drake for the ChaMP; 2002, private communication; Kim et al. 2003). A very soft emission component (0.2­0.3 keV) was reported in very X-ray­faint early-type galaxies (Kim et al. 1992, 1996; Fabbiano et al. 1994a), and its nature (from hot ISM or from stellar sources) has been debated

(e.g., Pellegrini & Fabbiano 1994). It has also been suggested that LMXBs might be the cause of this very soft emission, based on ROSAT and ASCA spectra of bright point sources in M31 and NGC 4697 (Irwin & Sarazin 1998; Irwin, Sarazin, & Bregman 2000). Chandra data exclude this latter hypothesis (the present results; see also Irwin et al. 2002).
2.4.2. Nucleus

As discussed in xx 2.2 and 2.3, a hard nuclear point source is clearly detected in the spatial analysis of the region where the diffuse emission is also most intense. We have fitted the spectrum from the central 500 of NGC 1316 with a power-law model for the AGN plus a MEKAL model for the hot ISM. The spectrum is well reproduced by this two-component model (reduced 2 of 0.65 for 59 degrees of freedom). The best-fit kT of the thermal component is 0.62 (ô0.02) keV, and the best-fit photon index of the AGN component is 1.76 (ô0.2). The metal abundance of the hot ISM was assumed to

TABLE 5 Spectral Fitting of Diffuse X-Ray Emission in NGC 1317 (r < 2000 ; Total Counts = 553) NH (1022 cmþ2) 0.00 0.14 0.13 0.00 (0.03) (0.02) (0.02) (0.02) FX kT1 0.33 0.31 0.31 0.32 (0.04) (0.03) (0.04) (0.03) Z 1.00 0.04 (0.01) 1.00 1.00 kT2 Total 0.53 0.58 0.58 0.72 Component 1 Component 2
2 reduced

Modela 1 2 3 4 .............. .............. .............. ..............

(2/dof) 21.1/21) 7.3/20) 7.3/19) 12.4/20)

0.33 (0.04) 5.00

0.28 0.46

0.30 0.27

1.00 0.37 0.39 0.62

(= (= (= (=

Note.--Errors in parentheses are at the 90% confidence level for one interesting parameter. a Model 1: one-component model; MEKAL with fixed Z. Model 2: one-component model; MEKAL with varying Z. Model 3: twocomponent model; MEKAL + bremsstrahlung. Model 4: two-component model; MEKAL + bremsstrahlung (with fixed kT2 ¼ 5:0). b F is in unit of 10þ13 ergs sþ1 cmþ2 in a 0.3­8.0 keV energy band. X


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Fig. 7.--X-ray color-color plot of point sources within D25 of NGC 1316. Sources with more than 50, 30­50, and 20­30 counts are denoted by filled circles, open circles, and stars, respectively. The brightest source (the ULX) is marked separately. The grid covers photon index þph ¼ 0­4 ( from bottom to top) and N ÏH÷ ¼ 1020 ­1022 ( from right to left). The two points on the right indicate the X-ray colors of the northern blob and the surrounding region at the similar distance from the center.

be solar (this is consistent with the constraints set in 2.4.4 on the metal abundance). The contribution from the power-law component is FX ¼ 1:3Ïô0:2÷á 10þ13 ergs sþ1 cmþ2 in 0.3­ 8.0 keV, which is in excellent agreement with the estimate from the radial profile analysis (in x 2.3). For comparison, spectral fitting with single-component models with either fixed or varying metal abundance were

also performed, and the results are shown in Tables 3 and 4 and Figure 8. A single-component model with best fit Z ¼ 0:14 Z also gives a formally acceptable fit, with a reduced 2 of 1.1 for 60 degrees of freedom. However, it is obvious from Figure 8 that the model predictions are systematically lower than the observed data at E > 2 keV. In contrast, the two-component model suggested by the image

Fig. 8.--Spectral fitting at the central bin (r < 500 ) with (a) a single-component MEKAL model with solar abundance, (b) a single-component MEKAL model with varying abundance, and (c) a two-component model with MEKAL (green)+power law (blue).


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(thermal gas+power law) not only has a lower reduced 2, but also reproduces the observed data well in the full energy range. Given the signal-to-noise ratio of the data, Z cannot be constrained in this case. This demonstrates that the spectral results depend critically on the adopted emission model (as pointed out in, e.g., Kim et al. 1996). We address this point further later in this paper.
2.4.3. Diffuse X-Ray Emission: Hot ISM and Undetected LMXBs

After excluding detected point sources, we have extracted spectra from the diffuse X-ray emission in three different annuli, with galactocentric radii between 500 and 6000 (see Tables 3 and 4). Because of the resolution of Chandra, the nuclear AGN does not contribute at r > 500 (Fig. 6), and the diffuse X-ray emission in these annuli is likely to be mostly from the hot ISM and undetected LMXBs. The observed spectra are well reproduced by a thermal gas (MEKAL) for the hot ISM+bremsstrahlung (or power-law) model for undetected LMXBs. The best-fit kT of the soft component has similar values in each annulus for all the applied models. While the kT of the innermost annulus is 0.63 keV (with a 0.03 keV uncertainty), consistent within the errors with that of the second annulus, our results suggest a general decrease of the temperature with increasing radius. We find kT ¼ 0:50 keV at r ¼ 3000 ­6000 . For all the fits, the reduced 2 is between 0.7 and 1.0. As was shown in the case of the nuclear spectrum, single thermal component models may give a formally acceptable result for very low abundance values. However, a systematic residual at the high energies points out the presence of a hard LMXB contribution (see Fig. 9, for the r ¼ 500 ­1500 annulus). We see a similar trend in the outer radial bins, but the excess at the higher energies is getting weaker. At radial bins of r ¼ 1500 ­3000 and r ¼ 3000 ­6000 , the formal statistics of spectral fitting do not favor a two-component model over a one-component, low-abundance model. However, based on our analysis of the two inner bins, we adopt the twocomponent model. In the two-component model, the hard component contributes about 25% of the total emission. In the region (r ¼ 2000 ­6000 ) where both X-ray emission components from the hot ISM and LMXBs can be measured, the X-ray contribution from the detected point sources is about 30% of the total X-ray emission. As discussed in x 3, the total X-ray luminosity of the hidden population of LMXBs can be 40%­100% of that of the detected LMXBs, depending on

the lower limit of XLF. Therefore, the expected contribution from the hidden LMXBs is about 12%­30%, which is in good agreement with the result estimated by the spectral fitting (25%). The relative contribution from the hard component to the total X-ray emission is more or less constant in the three radial bins, indicating that the amount of the hard component decreases with increasing radius, as expected if it comes from LMXBs. However, because of the uncertainties, it is statistically indeterminate whether the radial decrease is steeper than that of the diffuse X-ray emission and as steep as that of the detected point sources (as discussed in x 2.3).
2.4.4. Metal Abundance of the Hot ISM

The one-component model fit gives a very low value for the metal abundance of the hot ISM (Z ¼ 0:21 Z, with a formal 90% error of 0.04), but as we discuss in the previous section, this model does not represent well the higher energy data, where excess emission can be seen (Fig. 9), suggesting an undetected population of LMXBs. The metal abundance of the ISM is not well constrained with the two-component model, where this hard component is also fitted to the data, although in all cases solar values of the metal abundance (Z) are allowed by the fit. To improve the constraints on Z, we have performed spectral fitting by (1) fixing the parameters of the harder spectral component, using the values determined in x 2.4.1 for the integrated point source spectrum; and (2) combining spectra from different annuli. In both cases, we obtain an acceptable range for Z of $0.25 to $1.5 Z. However, both of these approaches disregard the spectral complexity that is suggested by our radial-annuli­based analysis. As shown in Tables 3 and 4, although the temperature of the soft component does not change much (DkT $ 0:12 keV in three radial bins between 500 and 6000 ), the temperature change is statistically significant at the 6 level, given the very small error of the measured temperature in each bin ("kT ¼ 0:03­0.04 keV at the 90% confidence level). Therefore, to fit the combined spectra extracted from the three annuli between 500 and 6000 , a proper model has to include at least three emission components (1 hard + 2 soft components). In this three-component spectral fit, the acceptable range of Z is 0.25­1.3 Z (at 90% confidence). Previous measurements of the metal abundance of the hot ISM of NGC 1316, from the analysis of ASCA spectra, are reported by Iyomoto et al. (1998) and Matsushita,

Fig. 9.--Spectral fitting at the radial bin of r ¼ 500 ­1500 (all detected point sources excluded from the spectrum) with (a) a single-component MEKAL model with solar abundance, (b) a single-component MEKAL model with varying abundance, and (c) a two-component model with MEKAL (green)+bremsstrahlung (blue).


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Ohashi, & Makishima (2000). ASCA SIS had a spectral resolution similar to that of Chandra ACIS, but a very large (arcminute) beam, so that no spatial discrimination of spectral emission components was possible. Iyomoto et al. (1998) found a slightly higher temperature (kT ¼ 0:77 ô 0:04 keV), but a much lower abundance (Z ¼ 0:11 ô 0:06 Z) than we find with Chandra. Note that the quoted (formal statistical) errors of both kT and Z are extremely small, and exclude the allowed parameter range from our present analysis. To do a direct comparison of our results with those of Iyomoto et al. (1998), we have extracted an integrated Chandra spectrum from a 10 circular region (including the AGN and detected point sources), to simulate the lack of spatial resolution of ASCA. Using the same model as theirs (Raymond thermal gas + power law with NH fixed at 1:5 á 1020 cmþ2) and the same energy range with a lower limit at 0.6 keV (ASCA was not sensitive below 0.6 keV), we were able to reproduce their results with the best fit Z ¼ 0:1 Z. The spectral fit is statistically good, with 2 ¼ 124 with 143 degrees of freedom. We note that the same model overpredicts at the low energies (0.3­0.6 keV) by as much as 50% and the statistics becomes worse, 2 ¼ 147 for 137 degrees of freedom, if estimated in the energy range of 0.3­5.0 keV. This result shows that there are no substantial calibration problems that may affect these comparisons. Our different conclusions are based on the unequivocal knowledge of spectral complexity that we can derive thanks to the spatial resolution of Chandra, which is guiding our choice of spectral models. Moreover, our ISM data, while containing some contamination from undetected LMXBs, are by and large the cleanest obtainable. Our results are consistent with the more recent conclusions (again from ASCA data) by Matsushita et al. (2000), who showed that more complex models could produce near solar abundances. We do not address the issue of nonsolar abundance ratios for Fe and elements, and of the uncertainties in the atomic spectral codes; these were suggested by Matsushita et al. (2000) as possible ways of obtaining Fe abundances closer to solar (as expected from the stellar metallicities, e.g., Arimoto et al. 1997). Given the comparable spectral resolution, their considerations still apply to all X-ray CCD data.
2.4.5. Spectrum of the `` Northern Blob ''

X-ray emission is soft (0.3­0.4 keV). The soft X-ray spectrum is consistent with thermal emission from a hot ISM. Given the poor counting statistics, we cannot comment on a LMXB contribution to the extended emission. The X-ray colors of the central source of NGC 1317 are consistent with the spectral fitting results, suggesting soft X-ray emission with C21 ¼ 0:27 ô 0:03 and C32 ¼ 0:83 ô 0:03, which would place this source near (slightly above) the blue triangle in Figure 7. The second brightest source (CXUO J032246.1þ370552) appears to have a relatively hard spectrum (suggesting that it is a LMXB associated with NGC 1317), with C21 ¼ þ0:28 ô 0:2 and C32 ¼ 0:73 ô 0:1, which approximately place it in Figure 7 in the middle of point sources found in NGC 1316. Its luminosity (LX ¼ 5 á 1038 ergs sþ1; Table 1) is consistent with a luminous LMXB.

3. THE XLF AND THE HIDDEN POPULATION OF POINT SOURCES

As described in x 2.2, an off-center, extended blob of X-ray emission was found at 3000 ­6000 north from the nucleus (Fig. 2). Its X-ray emission appears to be softer than the surrounding region (see Fig. 4). The X-ray colors confirm this softness. In Figure 7, we compare the X-ray colors from the northern blob (red square) and those from the annulus at the similar radius (blue triangle), r ¼ 3000 ­6000 , after excluding both the northern blob and detected point sources. The difference in the X-ray colors is consistent with the fact that the X-ray emission from the blob is softer. We discuss the possible nature of this off-center extended blob in x 5.3.
2.4.6. NGC 1317

As reported in x 2.1, three sources are associated with NGC 1317: an extended source centered on the galaxy, and two pointlike sources within the D25 ellipse (Table 1). The X-ray spectrum of NGC 1317 was extracted within a 2000 radius. Although the spectral fitting (Table 5) does not constrain well all the spectral parameters, it suggests that the

To determine the XLF of the point sources in NGC 1316, we have used 66 sources. These are the sources detected in CCD S3 at r > 2000 , to avoid the region of most intense diffuse emission and possible source confusion. We excluded four sources detected in CCD S2, to avoid the effect of different instrumental responses in the determination of flux limits. The cumulative XLF is shown in Figure 10, where both the binned (open squares) and unbinned (dotted line) distributions are plotted. The lowest luminosity point corresponds to the lowest luminosity sources detected in NGC 1316. A single power-law model was used to reproduce the data with count rate above 0.6 count ksþ1 (corresponding to LX > 1:2 á 1038 ergs sþ1), where completeness starts to drop (see below). Because errors in cumulative counts are not independent, we have applied the maximum likelihood method to fit the unbinned data and the minimum 2 method to fit the binned data. The best-fit power-law slopes determined with these two approaches are similar: þ1.32 (ô0.05) with the minimum 2 and þ1.25 with the maximum likelihood method. These values are consistent with those found in other early type galaxies (e.g., Sarazin et al. 2000), but much steeper than those in spirals and star burst galaxies (Prestwich 2001; Zezas & Fabbiano 2002). The XLF becomes flatter with decreasing source count rate below 0.6 count ksþ1. We have investigated this effect further to ascertain if it may be due to a physical break in the distribution of source luminosities (e.g., as suggested by Sarazin et al. 2000 and Blanton, Sarazin, & Irwin 2001 in other early-type galaxies) or may result from biases affecting the detection threshold of the data. We have explicitly considered two types of errors that may affect the lower count rate detections, and we have corrected the XLF accordingly: type I error is the probability of finding a spurious source, and type II error is the probability of misssing a real source. Large sets of simulations were performed (using the MARX simulator6) to quantitatively determine type I and II errors. For the determination of type I error, we have also used publicly available, long-exposure archival Chandra data to complement the simulation study, by splitting the longexposure data into multiple short ones to test how many false sources are identified in short-exposure data, but not
6

Available at http://space.mit.edu/CXO/MARX.


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Fig. 10.--X-ray luminosity function (XLF) of point sources within D25 of NGC 1316. The binned and unbinnned data are denoted by open squares and a dotted line, respectively. The solid histogram indicates the model prediction with a single power law, fitted at a count rate higher than 0.6 counts ksþ1. Three red squares and blue triangles at the lowest LX bins represent the XLF corrected using two different approaches for estimating incompleteness in source detection (see text in x 3 and Appendix).

in the long-exposure data. This second approach could in principle be affected by source variability, so a greater `` spurious`` detection may be expected than when using simulated data. We have found that type I error is always as good as or better than what is expected based on the threshold parameter in WAVDETECT. With the selected threshold of 10þ6, the number of spurious sources per CCD is 1 or less. On the other hand, type II error (the incompleteness effect) is more complex and varies significantly as a function of source count, background count, off-axis distance, and detection threshold. We estimated the incompleteness corrections in two different ways (see the Appendix for details): 1. Forward correction.--We estimated from simulations the detection probabilities for different source counts at different off-axis distances and for a range of background (+diffuse ISM) emission. This was done for nine galactocentric annuli with radii ranging from 2000 to 36000 . We then added corrections for the radial variation of the number of detected point sources (roughly following a rþ1 distribution) as determined in x 2.3. Corrections were also applied for the uneven sky coverage within the CCD S3 chip and for telescope vignetting (both included in the exposure map). The appropriate correction factor, including all the above effects, was applied to each bin of the differential XLF, from which a corrected cumulative XLF was then derived. This

exercise showed that incompleteness can be substantial: 50% for a typical source of 15 counts with background of 0.05 counts per pixel at 50 off-axis (see Appendix). 2. Backward correction.--we measured the correction factor, directly applicable to the cumulative XLF, by adding one by one a large number of simulated sources to the real image data and determining whether each one could be detected. In both approaches, no assumption was made on the behavior of the XLF below our detection threshold. In Figure 10, we plot both corrected XLFs; the forward correction is marked by red squares and the backward correction by blue triangles. The two corrections are consistent with each other and clearly demonstrate that the single power law (solid histogram), which was determined from the uncorrected XLF at LX > 1:2 á 1038 ergs sþ1, does fit well the corrected data. In conclusion, the apparent flattening of the XLF of NGC 1316 can be fully accounted for by incompleteness, and we find no evidence of breaks, down to source luminosities of $3 á 1037 ergs sþ1. At the high LX end, as the number of sources decreases rapidly with increasing LX, we cannot statistically exclude a possible break at LX > 5 á 1038 ergs sþ1, although it is not required by the data. Finoguenov & Jones (2002) reported ax XLF break at 5 á 1038 ergs sþ1 in M84, an elliptical galaxy in the Virgo Cluster, which could be reconciled with the Eddington limit by reducing LX by a factor of 0.5 by


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adopting a softer spectrum than the average spectra of point sources. However, we do not see any concentration of point sources with such soft spectra (see Fig. 7). The contribution of the hidden population of LMXBs to the observed X-ray emission depends on the low-luminosity XLF. As seen in the bulge of M31, it is possible to have a break at LX $ 1037 ergs sþ1 (Kong et al. 2002). If the XLF continues as an uninterrupted power law down to 1037 ergs sþ1, the total X-ray luminosity of the hidden population of LMXBs of NGC 1316 would be comparable to that of the detected sources. If the XLF has a break at the lowest observed LX (i.e., $3 á 1037 ergs sþ1), the luminosity ratio of hidden to detected sources is about 0.4. As demonstrated in x 2.4.3, the amount of hard component required in the spectral fitting of the diffuse X-ray emission is fully within this acceptable range. We have applied the same technique of completeness correction to other early-type galaxies for which Chandra data are publicly available. In general, near the center of earlytype galaxies, where the PSF is usually smallest, as the galaxy center is mostly likely at the focus, the strong diffuse emission considerably reduces the detection probability. On the other hand, at the outskirts, the PSF becomes considerably larger, and hence the detection probability becomes lower. So far we have found no clear case in which a broken power law is required. The results will be reported elsewhere (Kim et al. 2003).
4. SUMMARY OF EMISSION COMPONENTS

The Chandra observations of NGC 1316 have bearing on several questions. NGC 1316 is an X-ray­faint elliptical galaxy, and therefore our results have direct relevance for our understanding of the nature of the X-ray emission of this type of galaxies (see Fabbiano 1989). NGC 1316 is also the Fornax A radio galaxy, and therefore we can explore the interaction of the radio jets with the hot ISM in this system, and we can study the X-ray properties of the active nucleus. Finally, NGC 1316 is likely the product of a merger (e.g., Schweizer 1980), and therefore our results are relevant for understanding merger evolution. In what follows we will address these three main topics in turn. 5.1. NGC 1316 as an X-Ray Faint Elliptical Galaxy While hot ISM was discovered over 20 years ago in E and S0 galaxies (Forman et al. 1979), the properties of this medium and its evolution have been the subject of heated discussion (see e.g., Fabbiano 1989; Ciotti et al. 1991; Eskridge et al. 1995a, 1995b; Arimoto et al. 1997). X-ray­ faint E and S0 galaxies, of which NGC 1316 is one, were particularly debated. These are galaxies with X-ray to optical luminosity ratios 100­1000 times smaller than those of hot-halo­dominated Virgo galaxies. A question that was raised early on is the role of the hot ISM in the overall X-ray emission of these galaxies versus that of LMXBs (ISM dominant: e.g., Forman, Jones, & Tucker 1985; LMXBs dominant: Trinchieri & Fabbiano 1985; Canizares et al. 1987; both present: Fabbiano et al. 1994b; Pellegrini & Fabbiano 1994). With the advent of CCD X-ray spectrometers (ASCA SIS), it became clear that the X-ray spectra were complex, with a thermal hot ISM component and a harder component, possibly from LMXBs (Matsushita et al. 1994). Still, the lack of spatial resolutions made the interpretation of these data ambiguous at times: in particular, a low-luminosity AGN could also contribute to the hard component; LMXBs were suggested to contribute to the soft emission (Irwin & Sarazin 1998). Moreover, the issue of the metal abundance of this hot ISM remains controversial and open (see Arimoto et al. 1997; Matsushita et al. 2000), and ASCA could not establish the spatial/spectral properties of this medium, which are important for understanding its physical state (e.g., Pellegrini & Ciotti 1998). NGC 1316 joins a growing body of E and S0 galaxies observed with Chandra at subarcsecond resolution. With these data we now have uncontroversial proof of the

The X-ray fluxes and luminosities of the different emission components of NGC 1316 are summarized in Table 6. For the detected LMXBs, all point sources are included except two sources at the center of NGC 1316, which may be associated with features of the ISM (x 2.1). We estimate that $10% of LMXBs are outside the field of view in CCD S3, based on the spatial distribution of point sources detected in CCD S3. We have corrected the entries in the table for this effect. We give two estimates of the X-ray emission from the undetected LMXBs, obtained by taking the lower limit of the XLF at either 1 á 1037 or 3 á 1037 ergs sþ1. We note that the integrated LX of the undetected LMXBs could be as large as that of the hot ISM, although their total counts is smaller because of the harder LMXB spectrum. We also note that the error on LX caused by the uncertainty on the hidden LMXB contribution is much larger than the formal statistical error.

TABLE 6 X-Ray Luminosities of Individual Components FX (10þ13 ergs cm LX (1040 ergs sþ1) 0.51 2.3 3.1 0.92­2.3 2.2­2.7 6.4­7.3

Component AGN....................................................... LMXB (detected) .................................... Diffuse (gas + undetected LMXB) .......... Undetected LMXB ................................. Gas only.................................................. Total .......................................................

Net Counts 520 2130 6400 840­2100 4460­5620 9050

þ2 sþ1

)

1.3 5.8 7.8 2.3­5.8 5.4­6.8 16.2­18.3

Note.--FX and LX are in a 0.3­8 keV energy band. ECF ¼ 6:0 á 10þ15 , 6:7 á 10þ15 , and 3:0 á 10þ15 for 1 count ksþ1 are used for AGN, LMXB, and gas components, respectively. For the diffuse emission (gas+undetected LMXBs), ECF for gas was used. About 10% of LMXBs are added because of the limited field of view. The X-ray emission from the undetected LMXBs is estimated by assuming the lower limit of XLF at 1­3 á 1037 ergs sþ1.


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existence of populations of X-ray binaries in all E and S0 galaxies and of their large contribution to the emission of X-ray­faint galaxies (see Sarazin et al. 2000, 2001; Blanton et al. 2001; Angelini, Loewenstein, & Mushotzky 2001). In NGC 1316, we detect 81 nonnuclear point sources, with a surface brightness distribution following that of the optical stellar light. These sources have the hard (kT $ 5­6 keV) spectrum characteristic of LMXBs, and luminosities in the range 2 á 1037 to 2 á 1039 ergs sþ1. Around 35% of these sources (with one ULX) have LX > 2 á 1038 ergs sþ1, the Eddington luminosity of neutron star X-ray binaries. One source is a supersoft X-ray source (SSS). Five sources have globular cluster (GC) counterparts (Table 1); sources in GCs are found frequently in ellipticals, and GCs have been suggested as the birthplace for a large fraction of LMXBs in these galaxies (White, Sarazin, & Kulkarni 2002). In contrast to earlier reports for other early-type galaxies (e.g., Sarazin et al. 2000), we find that the XLF of the NGC 1316 sources does not have a strong break at the Eddington luminosity of an accreting neutron star, but appears to follow an uninterrupted $1.3 steep power law down to our detection threshold luminosity of $3 á 1037 ergs sþ1, once incompleteness corrections are applied. The presence of a substantial number of faint LMXBs is also suggested by the spectra of the diffuse emission within a 500 ­6000 annulus: after removal of all the detected point sources in this region, they still contain a hard component, presumably from undetected LMXBs, accounting for $25% of the emission. Given that the emission at the outer radii is dominated by the pointlike component in NGC 1316 (x 2.3), the total LMXB contribution to the emission of this galaxy is larger. Extrapolating the XLF at lower luminosities, the total (detected and undetected) LMXB emission could account for $1/2 to $2/3 of the total X-ray luminosity of NGC 1316, depending on the low-luminosity break of the XLF (Table 6). The larger estimate was calculated for a XLF break at 1 á 1037 ergs sþ1, analogous to that reported in the bulge of M31 by Kong et al. (2002). The Chandra data also show hot ISM in NGC 1316, confirming earlier ROSAT results (KMF). This hot ISM is more centrally concentrated than the LMXB and stellar light distributions, and appears to be cooler at larger radii. The steep X-ray surface brightness profile of the diffuse emission, the average temperature of the hot ISM (kT $ 0:5­0.6 keV) and the radially decreasing temperature profiles we derive from our spectral analysis, together with the low X-ray luminosity ($2:5 á 1040 ergs sþ1), could be consistent with the Pellegrini & Ciotti (1998) picture of partial wind flows for X-ray­faint ellipticals. The abundance of heavy elements has been identified as one of the key quantities for our understanding of the evolutionary status of the hot ISM in terms of the supernova rate (Ia and II), IMF, mass ejection, and onset of galactic winds (e.g., Renzini et al. 1993; Matteucci & Gibson 1995). Yet its measurement is difficult. While the ACIS spectral resolution is comparable to that of the ASCA and XMM CCD detectors, the spatial resolution of Chandra can remove some of the ambiguity in the choice of spectral models for spatially/ spectrally complex sources, such as galaxies. Different models may all give acceptable spectral fits, and the accepted practice is to adopt the simplest possible model; however, the answer may not be astrophysically meaningful, because of the complexity of the sources we are attempting to fit. Fits

of the ROSAT and ASCA data with single-temperature Raymond-Smith spectra (+hard component) suggested a hot ISM almost totally devoid of metals in X-ray­faint galaxies (e.g., Awaki et al. 1994; Loewenstein et al. 1994; Davis & White 1996; Matsumoto et al. 1997; Iyomoto et al. 1998 for NGC 1316), while more complex models allowed a metal content more in keeping with the stellar metallicities (e.g., Trinchieri et al. 1994; Kim et al. 1996; Buote & Fabian 1998; Matsushita et al. 2000). As shown in x 2.4.4, we can remove some of this ambiguity in NGC 1316 by excluding the regions of the data cube occupied by detected pointlike sources (AGNs and LMXBs) from the spectral data and establishing the existence of variations (in $1000 radial scales) of the temperature of the hot ISM. While we do not address uncertainties in the spectral codes, which persist in all the spectral analyses of thermal X-ray emission (see Matsushita et al. 2000), our analysis, guided by the highresolution images of Chandra, convincingly excludes the possibility of extremely low metal abundances in the hot ISM (see Iyomoto et al. 1998), giving an acceptable (90% confidence) range of Z ¼ 0:25­1.3 Z. However, we note that the Fe abundance is still lower than what might be expected (e.g., Arimoto et al. 1997), particularly if the partial wind is driven by a Type Ia supernova. A final topic of considerable debate has been the ability to measure the gravitational mass of E and S0 galaxies, based on the assumption of hot halos in hydrostatic equilibrium (see, e.g., Fabbiano 1989; Trinchieri, Fabbiano, & Canizares 1986). In particular, it was pointed out by the above authors that this method would not apply (or at least would be extremely uncertain) in the case of X-ray­faint galaxies. This is certainly true in the case of NGC 1316, for which a mass of 2:0 á 1012 M was estimated, based on the Einstein data (Forman et al. 1985). The mass measurement based on the equation of hydrostatic equilibrium (see, e.g., discussion in Trinchieri et al. 1986) hinges on four quantities (outer radius of the halo, temperature, density, and temperature gradients at this radius). In NGC 1316, we have found that the X-ray binaries dominate the emission at the outer radii, while the gas extends out to $ 6000 (5.4 kpc for the distance adopted in this paper). Taking into account the different distance used by Forman et al., the radius of the halo used in the mass estimate was $19 kpc, comparable to the radius of the region within which LMXBs are detected. The temperature of the halo was assumed to be $1 keV (we now know it is 0.5 keV). Clearly, using data with less angular and spectral resolution than Chandra (1) we would not be able to separate point sources from diffuse emission, giving a mistaken larger radius for the hot halo, and a more relaxed radial distribution; (2) the temperature of the halo may appear larger than it really is, because of contamination with the harder LMXB emission, if these cannot be removed spatially or spectrally (the CCD resolution of ASCA helped on the spectral analysis for the first time); and (3) the halo may not be in a state of hydrostatic equilibrium, if, for example, it is subject to winds at the outer radii, as it may be the case, based on the present data. These types of uncertainties are common to all pre-Chandra mass measurements of X-ray­faint E and S0 galaxies: because of the problems exemplified in the case of NGC 1316, these measurements would tend to err in excess, even if the hot ISM were in hydrostatic equilibrium. Caution should be exercised even when interpreting XMM data, although the XMM moderate spatial resolution and CCD


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spectral capabilities allow a better discrimination than any of the pre-Chandra missions. 5.2. The Fornax A Radio Galaxy Figure 3 shows the direction of radio jets (from the 1.5 GHz VLA map of Fig. 2b in Geldzahler & Fomalont 1984) superposed on the X-ray image. The radio jets propagate along P:A: $ 120 and 320 , and slightly bend at their ends toward P:A: $ 90 and 270 , respectively (Geldzahler & Fomalont 1984). It is clearly seen that the radio jets in the projection (1) run perpendicular to the direction of the subarcminute-scale northeast-southwest elongation of the central X-ray distribution, which is also the direction of the optical figure, and (2) propagate through the valleys of the X-ray emission, confirming the results of the ROSAT HRI observations (KFM). This alignment suggests that the X-ray valleys are cavities in the hot ISM caused by exclusion of hot gas from the volumes occupied by the radio jets. Similar relations between the radio jets/lobes and X-ray features have been reported in the Chandra observations of NGC 4374 (Finoguenov & Jones 2001), Hydra A (McNamara et al. 2000), the Perseus cluster, (Fabian et al. 2000), and Abell 4095 (Heinz et al. 2002). In particular, the hourglass-like feature seen in the core of Abell 4095 is similar to the X-ray feature in NGC 1316, although only one of (possibly) two X-ray cavities in Abell 4095 coincides with the radio emission. Based on the hydrodynamic simulations of Reynolds, Heinz, & Begelman (2001), Heinz et al. (2002) have interpreted the hourglass feature in Abell 4095 as a sideways expansion of the jet's surface caused by a compression wave (or sonic boom), which would follow after driving a strong shock. However, in NGC 1316 the jets appear to escape the denser halo. It is therefore not clear whether a sonic boom could explain the northeast-southwest elongation. This elongation could simply reflect the hot ISM sitting on the local, spherically asymmetric potential because it also follows the major axis of the galaxy. Although NGC 1316 has luminous radio lobes, the radio emission from the AGN is relatively faint. Fornax A contains a relatively weak radio core with a total power of $1038 ergs sþ1 (Geldzahler & Fomalont 1984). We note that the current nuclear radio power is too weak to sweep the hot ISM out of the X-ray cavities, as it would take longer than $10 Gyr for the minimum energy required by pV $ 1056 ergs, where the pressure was taken from KFM. This indicates that the nuclear activity was much stronger in the past, as suggested by Ekers et al. (1983). Mergers, which took place a few Gyr ago, might have ignited the AGN activity, which in turn swept out the hot gas and also powered the huge radio lobes. The AGN in NGC 1316 has a LINER-type spectrum (Veron-Cetti & Veron 1986; Baum, Heckman, & van Breugel 1992) and HST observations have revealed a nuclear UV-bright point source (Fabbiano, Fassnacht, & Trinchieri 1994a). With our Chandra ACIS observation we have discovered the X-ray counterpart of this nuclear emission, which is prominent in the hard-band image (Fig. 4). The nuclear component is also required to fit the radial profile (Fig. 6) and the X-ray spectrum of the nuclear region (Fig. 8). For this source we have measured a flux FX ¼ 1:3 á 10þ13 ergs sþ1 cmþ2 (in 0.3­8 keV) and a luminosity LX ¼ 5 á 1039 ergs sþ1 (see xx 2.2 and 2.4.2), consis-

tent with the upper limit estimated by KFM. The spectrum of this source is well fitted with a power law with photon index þ $ 1:7. Based on the relationship between MBH and the stellar velocity dispersion (Tremaine et al. 2002), the estimated mass of the nuclear black hole of NGC 1316 is about MBH ¼ 1 2 á 108 M for ¼ 221 km sþ1 (Kuntschner 2000). The X-ray luminosity of the nuclear source then corresponds only to 10þ6 LEddington . Both luminosity and spectral characteristics are reminiscent of those of the X-ray­faint nucleus of IC 1459 reported in Fabbiano et al. (2003), to which we refer for further discussions of this type of source (see also Ho et al. 2001; Pellegrini et al. 2002). We are conducting multifrequency VLA observations to obtain high S/N radio images of the nucleus and jets with a resolution comparable to that of the Chandra observations. We will report in-depth comparison between the X-ray and radio data and their implications in another paper. 5.3. Features and History of the Hot ISM NGC 1316 is an X-ray­faint elliptical galaxy, i.e., it has relatively little hot ISM, much less than would be expected from steady accumulation of the gas shed by evolving stars during an undisturbed galaxy lifetime (see Fabbiano 1989; Eskridge et al. 1995a, 1995b). Since NGC 1316 is the likely product of recent mergers (Schweizer 1980), this lack of hot ISM could be related to its recent merging history. KMF noted that the total amount of the hot ISM ($109 M ) is comparable to what would have been accumulated for a few Gyr. Other merger remnant galaxies have also been found to be X-ray­faint (Fabbiano & Schweizer 1995; Hibbard et al. 2001). A close look at a nearby merger remnant, the X-ray­faint S0 NGC 5128 (Cen A), with Chandra, has revealed a complex distribution of cold and hot ISM (Karovska et al. 2002). Similarly, in NGC 1316 the Chandra images confirm the complex distribution of the hot ISM suggested by ROSAT (KFM). Besides the cavities created by the expanding radio jets that we have just discussed, the hot ISM presents other fine structures that may be indicative of either absorption by cold dusty ISM in the line of sight but within the parent galaxy, or a multiphase ISM, in which hot and cold phases are intermingled. This is shown by Figure 11, where we compare the Chandra X-ray surface brightness distribution with the archival HST WFPC2 image taken with a F450W filter (central wavelength at 4520 ° ° A and bandwidth of 958 A). Many prominent dust features are visible in the HST WFPC2 image, and we indicate them with green lines in the figure. They correspond to the central part of the lower resolution dust lane map of Schweizer (1980). Some dust features are seen where the X-ray surface brightness is reduced, suggesting absorption. As discussed in x 2.2, we have found an off-center, 2­3 kpc extended blob of X-ray emission at 3000 ­6000 north from the nucleus, which is also cooler than the surrounding hot ISM (xx 2.2 and 2.4.3). We estimate a cooling time of about 2 Gyr for this feature. This cooling time is similar to the time of the latest merger event in NGC 1316 (Schweizer 1980; Ekers et al. 1983; confirmed by more recent optical studies of star clusters, Goudfrooij et al. 2001). It is therefore possible that the formation of the blob may be related to compression of the ISM during the last merging of NGC 1316. A similar off-center blob was seen in the Chandra observations of NGC 507. Given its position relative to the radio


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° Fig. 11.--HST WFPC2 image at 4520 A (F450W filter) of the central part (3600 á 3600 ) of NGC 1316 (left) and the Chandra X-ray image (right) plotted in the same scale. The green marks indicate the dust lanes seen in the HST image. North is to the top and east is to the left.

lobe, Forman et al. (2001) have interpreted it as being ISM displaced by the radio lobe. However, since the direction to the blob in NGC 1316 is almost perpendicular to that of the ratio jets/lobes, the cooling blob in NGC 1316 appears to be unrelated to the radio jets. The origin of the various phases of the ISM in early-type galaxies has been discussed since the early detection of cold/ warm ISM in forms of H i, far-IR, CO, dust lanes, and H (e.g., Jura et al. 1987; Kim 1989). The two options that have been advanced are that either the cold/warm ISM could be of external origin, accreted by way of merging and closeencounter episodes with other galaxies, or it could be the by-product of cooling hot ISM originating from internal stellar mass loss, e.g., via cooling flows (e.g., Knapp, Turner, & Cunniffe 1985; Kim et al. 1988). In NGC 1316, the kinematics of the ionized (Schweizer 1980) and molecular gas (Sage & Galletta 1993), compared to those of the stellar system (Bosma, Smith, & Wellington 1985), indicate that cold/warm ISM and stars are decoupled, suggesting an external origin for this phase of the ISM. This is not surprising, given the likely merging history of NGC 1316. Instead, since the hot ISM is likely to originate from stellar evolution (see review in Fabbiano 1989), we would expect it to share the stellar kinematics and to be decoupled from the cold ISM. This possibility was suggested by earlier works. With the ROSAT HRI data, we pointed out that the morphology of the larger scale distribution of the hot ISM suggests a disk co-aligned with the stellar system central X-ray flattening (KFM), and that the hot and cold ISM are not morphologically related (Mackie & Fabbiano 1998). A future deep Chandra observation of NGC 1316 would give us the means to explore this point further by examining in detail the properties of the interface between cold and hot ISM.
6. CONCLUSIONS

The high-resolution Chandra ACIS observations of the X-ray­faint merger remnant NGC 1316, the Fornax A radio galaxy, have provided an unprecedented look at this complex system. In summary:

1. We have confirmed the presence of cavities in the hot ISM related to the expanding radio jets, first suggested on the basis of a ROSAT HRI observation (KFM). 2. We have discovered a low-luminosity AGN (FX ¼ 1:3 á 10þ13 or LX ¼ 5 á 1039 ergs sþ1). Although the nuclear source is weak, its power-law spectrum is typical of luminous AGNs, with a best-fit photon index of 1.7. 3. We have found 81 point sources in NGC 1316 and three in the nearby galaxy NGC 1317. Their average spectrum is hard ($5 keV) and the radial distribution follows that of the optical light, indicating that most of them are LMXBs associated with the galaxy. Five of these sources have GC counterparts and one is supersoft; 35% of them (with one ULX) have X-ray luminosities in excess of the Eddington luminosity of an accreting neutron star. 4. The X-ray luminosity function (XLF) of the NGC 1316 sources is well represented by a single power law with a slope of þ1.3, which is consistent with those of other earlytype galaxies studied with Chandra (Sarazin et al. 2000) but much steeper than that of spiral or starburst galaxies (Prestwich 2001). The uncorrected XLF shows a flattening at the faint end, which is removed once corrections are applied for the incompleteness errors stemming from the local diffuse emission at small galactocentric radii and from the increasing PSFs at larger off-axis angles. Once these corrections are applied, the XLF follow an uninterrupted power law, with no breaks, down to a luminosity of $3 á 1037 ergs sþ1, indicating that there are still a considerable number of faint, undetected sources. Even without the incompleteness correction, the single power law is still applicable to the observed XLF down to 1038 ergs sþ1, at luminosities below the break at LEddington of neutron star binaries reported in other X-ray­faint elliptical XLFs (Sarazin et al. 2000; Blanton et al. 2001). 5. The radial profile of the diffuse X-ray emission varies at different position angles: it is steeper toward the east-west than the north-south. Regardless of P.A.s, the radial profile of the diffuse X-ray emission is much steeper than that of the optical light, unlike that of the LMXBs (see point 3 above). This means that the relative contribution of the


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KIM & FABBIANO pipeline processing and data analysis. We thank D. Harris for carefully reading the manuscript, V. Kashyap for measuring detection probability (Fig. 12), and A. Vikhlinin for suggesting a backward simulation.

LMXBs to the diffuse emission increases with galactocentric radius. At large radii, the diffuse emission is likely to be dominated by unresolved LMXBs rather than by the hot ISM. 6. Spectrally, the diffuse X-ray emission (extracted from narrow annuli and after subtracting all detected point sources) is well reproduced by two-component models: in the nuclear region, thermal optically thin gaseous emission plus an AGN power-law component; at larger radii, gaseous emission plus a hard component from the undetected LMXBs. The best-fit temperature for the gaseous component is kT $ 0:5­0.6 keV, with a small but statistically significant decrease (by 0.12 keV) from the center to 6000 . We constrain the metal abundance of the hot ISM to be in the range 0.25­1.3 Z (90% confidence). 7. The hot ISM presents a number of features that may be related both to interaction with the radio emission (the cavities) and to the recent merging history of NGC 1316 (Schweizer 1980). In particular, there is clear intermingling of cold and hot ISM in the central regions. We have also found a well-defined soft emission region (blob) at $4000 north from the nucleus. Given its cooling time of 2 Gyr, it could be a cooler blob falling into the center, formed at or after the recent merger. Overall, the relatively small amount of hot ISM in NGC 1316 is consistent with the observations of other recent mergers (Fabbiano & Schweizer 1995; Hibbard et al. 2001). The current radio power of the nucleus and jets is too weak to sweep out the hot gas out of the cavities, indicating that the AGN was more powerful in the past, around the time of the recent merger. The irregular morphology of this ISM and the interplay between hot and cold phases are also reminiscent of the recent Chandra results on NGC 5128 (Cen A), another nearby merger remnant (Karovska et al. 2002). These results (particularly points 2­6) have an important bearing on the interpretation of lower angular resolution data of early-type galaxies, both pre-Chandra, XMM, and of future planned missions (Constellation X, XEUS ). It is only with subarcsecond resolution that we can resolve the LMXB population and the low-luminosity nuclear AGN. This, coupled with the wide energy band and spectral resolution of ACIS, leads to a clear definition of the spatial and spectral properties of the different emission components. As a result, we can conclude with confidence that: (1) LMXBs are a dominant contributor in the X-ray­faint early-type galaxy NGC 1316 (see also Sarazin et al. 2000; Blanton et al. 2001 for other examples of X-ray­faint early-type galaxies). These results confirm the early inference based on Einstein and ROSAT observations (see Fabbiano 1989; Trinchieri & Fabbiano 1985; Canizares et al. 1987). (2) ROSAT and ASCA reports of an ISM devoid of metals in these galaxies were biased by the lack of a proper appreciation of the spectral complexity of these systems (as discussed by Matsushita et al. 2000), which becomes evident when a spatially resolved spectral analysis can be undertaken. (3) X-ray-based mass measurements for these systems (see Fabbiano 1989) that do not take into account the real distribution of the hot ISM (both spatially and spectrally, for which adequate spatial and spectral resolution are needed) are bound to be wrong and should not be attempted. This work was supported by NASA grant GO1­2082X. We thank the CXC DS and SDS teams for their supports in

APPENDIX INCOMPLETENESS CORRECTION
A1. FORWARD CORRECTION

The detection probability (type II error) is a complex function of background counts per pixel, different source counts, and off-axis distances. Large sets of simulations based on MARX were performed (V. Kashyap et al. 2003, in preparation) to establish the behavior of the detection probability in a wide parameter space. The results are illustrated in Figure 12: the detection probability decreases as the effective background rate (which in our case includes both field background and galactic diffuse emission) and the off-axis angle increase and as the source count decreases. Incompleteness could be as large as 50% for a typical source of 15 counts with background of 0.05 counts per pixel at 50 off-axis. In the Chandra observations of NGC 1316, the effective background ranges from 0.2 count per pixel at 2000 from the center of NGC 1316 to 0.03 count per pixel at 6000 and beyond. This is large enough to result in a significant amount of type II errors for weak sources. For the source counts corresponding to the three lowest luminosity bins of Figure 10, we have determined incompleteness-correction factors, applicable to the differential XLF, as summarized in Table 7. Detection probabilities were calculated for nine galactocentric radial bins (from 2000 to 36000 ), appropriate for the bin's off-axis angle and effective background emission. These detections probabilities are listed in the last three columns of Table 7. Then we applied three factors to correct for the considerations that (1) the number of point sources in unit area decreases as the distance from the galactic center increases (F1 in Table 7), (2) the outer part of the galaxy is not fully covered by CCD S3 (F2 in Table 7), and finally (3) the telescope vignetting and CCD response vary at different positions (F3 in Table 7). Weighted-mean correction factors for each luminosity bin were then determined by multiplying these factors in each radial bin, summing them together, and normalizing by the value similarly determined with detection probability equal to 1.0. The estimated correction factor in each bin is then applied to the differential XLF, and the cumulative XLF is derived from the corrected differential XLF. The three red squares in Figure 10 indicate the cumulative XLF with these corrections. The radial dependence of the detection probabilities in Table 7 reflects the effects of the variation in background level and PSF. We have excluded r < 2000 where the background is larger because of the more intense diffuse emission, and source confusion may also be an issue, because of the increased surface density of point sources. The detection probabilities increase with radius and peak between 6000 and 12000 , because of the decrease of the background (+diffuse) emission. At larger radii, the predominant effect is the increase of the PSF, which results in a significant decrease of the detection probability.


Fig. 12.--Detection probabilities as a function of background count with various source counts (from a few to $100) and off-axis distances: (a) on-axis, (b) 20 off-axis, (c)50 off-axis, and (d )100 off-axis.

TABLE 7 Correction Factors for the Last Three Bins of XLF Detection Probability rin (arcsec) rout (arcsec) Background Rate (counts pixelþ1) 0.12 0.09 0.07 0.06 0.04 0.03 0.03 0.03 0.03 Area (arcsec2) 1570 2198 2826 3454 33912 56520 79128 101736 124344 26897h 1.0 F1
a

F2

b

F3

c

Bin 1d 0.7 0.75 0.75 0.75 0.8 0.6 0.4 0.3 0.3 15746 0.58

Bin 2e 0.55 0.6 0.6 0.6 0.7 0.5 0.2 0 0 11868 0.44

Bin 3f 0.1 0.15 0.15 0.15 0.2 0.1 0 0 0 2611 0.09

20 ........... 30 30 ........... 40 40 ........... 50 50 ........... 60 60 ........... 120 120 ......... 180 180 ......... 240 240 ......... 300 300 ......... 360 Weighted sumg ........... Correction factor .......
a b c d e f g h

1000 714 555 455 250 156 114 89 74

1.0 1.0 1.0 1.0 1.0 1.0 0.94 0.79 0.70

716 717 718 714 714 591 415 388 334

Number of point sources in unit area (arbitrarily scaled). Area coverage within CCD S3 (arbitrarily scaled). Telescope vignetting (arbitrarily scaled). logÏcount rate÷ ¼ þ3:3; counts ¼ 9:8 15:6. logÏcount rate÷ ¼ þ3:5; counts ¼ 6:2 9:8. logÏcount rate÷ ¼ þ3:7; counts ¼ 3:9 6:2. Weighted sum is ô(detection probability á area á F1 á F2 á F3). Weighted sum with detection probability ¼ 1:0.


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Fig. 13.--Comparison of detected counts with input counts. The input source flux was selected randomly, according to a single power law, simulated with MARX, added to the real image, and then detected by WAVDETECT.

A2. BACKWARD CORRECTION

To confirm the incompleteness corrections, we have also run a simulation, based on the real, observed data of NGC 1316. This time we have determined the correction factor, directly applicable to the cumulative XLF, by adding a simulated source to the real image and determining whether it could be detected. To do this, we have selected an input source with a random flux based on a single power law XLF and with a random location based on the optical light distribution of NGC 1316. Note that the assumed XLF is not critical here, because we are only using the ratio of input and output numbers of sources (see Vikhlinin et al. 1995). We have then simulated the sources with MARX, added them one by one to the real image, and tried to detect them with WAVDETECT. As the real data are being used, those factors necessary in the forward correction (such as radial variations, sky coverage, etc.) are already taken into account and the ratio of input to output XLF can be directly used to correct the cumulative XLF. Figures 13­15 show the results of this simulation with 20,000 input sources. In Figure 13, we compare detected counts with input counts. Note that the relative difference increases as the count

decreases and the Eddington bias (detected counts tend to be larger than input counts because there are more fainter sources) is present at low counts (see also Vikhlinin et al. 1995; Kenter & Murray 2003). Because of the confusion with the strong diffuse emission and with other sources near the center of the galaxy, the detected counts are sometimes considerably different from the input counts. As with the real data analysis in x 2, we do not use sources at r < 2000 . Figure 14 shows the spatial distribution of simulated sources (green crosses). A red circle on a green cross indicates a detection. Only 1000 random sources are plotted, for visibility. This clearly demonstrates that many faint sources are undetected. Figure 15 exhibits the comparison of input (blue solid line) and measured (red dotted line) XLFs. It is very interesting to note that the measured XLF closely resembles the observed XLF in Figure 10, indicating that the flattening is not real. The ratio of detected to input number of sources is applied to correct the XLF in Figure 10 (red triangle). The two results of simulations are fully consistent and reconfirm the amount of incompleteness correction and the validity of an unbroken, single power law down to a few á 1037 ergs sþ1.


Fig. 14.--Spatial distribution of simulated sources (green crosses). A red circle on a green cross indicates a detection. Only 1000 random sources are plotted, for visibility. The abscissa and ordinate units are the same as the ACIS sky coordinate, i.e., 1 pixel ¼ 0 > 492.


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Fig. 15.--Comparison of input (blue solid line) and measured (red dotted line) XLFs. The ratio of detected to input numbers of sources is applied directly to correct XLF in Fig. 10 (red triangle).

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