... The spectroscopic modes of JWST NIRSpec and MIRI cover the main molecular bands of gas in planet-forming regions, tracing gas at temperatures of 100-1000 K. The integral field units of JWST will resolve the molecular emission in nearby protoplanetary disks, while the high sensitivity will allow observations of disks as far away as the Magellanic Clouds, constraining the chemistry of planet formation in a wide range of environments. ...

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• The State of the Gas and the Relation between Gas and Star Formation at Low
• Spitzer Analysis of H II Region Complexes in the Magellanic Clouds: Determining
• The CO-to-H2 Conversion Factor from Infrared Dust Emission across the Local

... High-resolution Herschel spectroscopy reveals the proto-planetary disk around the young star T Tau N . ... A study led by Linda Podio ( AstroFIt fellow at the Arcetri Observatory) with Inga Kamp (Kapteyn Institute, the Netherlands), Claudio Codella (Observatory of Arcetri) and other collaborators from Grenoble, UK and USA, makes use of high-resolution spectroscopic observations with HIFI on board the Herschel space observatory to characterize the disk around the young star T Tau N . ...

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• Arcetri Star-Formation Group Publications
• Arcetri Star-formation Group Research Topics

... High-velocity clouds (HVCs) were discovered by Muller, Oort & Raimond (1963) in the 21-cm line emission of neutral, atomic hydrogen. They are gas clouds which are characterised by high radial velocities incompatible with a participation in the rotation of our Galaxy. ... This suggestion was seized by Braun & Burton (1999) who identified 66 compact high-velocity clouds (CHVCs) with positional and kinematic characteristics being compatible with a distribution across the entire Local Group. ...

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• ATNF Colloquium
• Research - The high-velocity clouds of M31
• Australia Telescope Compact Array Home Page

The compression of the cloud of gas in star forming . ... These data have allowed us to create the dynamic model of the cloud of gas, around this object. ... The results on H2CO absorption lines (figure 1) have shown, that the central part of the cloud represents a clumped envelope of diameter 9 pc with radial velocity 20 km/s. The relation of radial velosity of absorption line and the whole object have allowed simple to define the direction of radial movement - itis compression. ...

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• Results scientific researchs 11
• Results scientific researchs LRS
• RESEARCH PROBLEMS of the LRS

All stars are formed deep inside molecular clouds. One of the current enigmas lies in the formation and evolution of molecular clouds, specifically the conversion from atomic to molecular gas. ... In July of 2005 GALFA mapped about 300 square degrees of the Taurus Molecular Cloud (TMC) complex yielding the largest high-resolution 21cm map of a star forming region, while using less than 40 hours of observing time. ...

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• Galactic Spiral Structure in H I Emission and Self-Absorption
• What is HISA?

... Prominent features include a small open cluster of stars, a diffuse red-glowing emission nebula , large lanes of obscuring gas and dust , and dense knots of dust and gas in which stars may still be forming. The open cluster of stars IC 1590 visible around the center has formed only in the last few million years. ... Publications with keywords: NGC 281 - emission nebula - open cluster . Publications with words: NGC 281 - emission nebula - open cluster . ... Emission Nebula IC 1396 . ...

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• Астронет > NGC 281: Cluster, Clouds, and Globules
• Fliers Around the Blue Snowball Nebula
• Molecular Cloud Barnard 163

... Search . ... Astrophysics Group . Research . ... Research and Instrumentation . ... While this seems an extraordinary endeavour, in light of what we have learnt about Solar System planets, only a handful of key ingredients are required to start characterising an exoplanet. ... The NGTS project is a partnership between the University of Cambridge, Queen?s University Belfast, University of Warwick, University of Leicester, Observatoire de Geneve, DLR (Berlin) and Universidad Catolica de Chile. ...

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• A 215 to 265 GHz spectral line survey of the Sgr B2 molecular cloud
• Astrophysics Group Stars ? Birth and Death
• Astrophysics Group Star Formation

... Shustov B.M., Wiebe D.S. Dust expelling from the Galaxy ( abstract from the journal ). Astronomy Reports , 1995, 39 , 578-586 [AZh, 72 , 650-659]. Wiebe D.S., Shematovich V.I., Shustov B.M. Chemical and dynamical evolution of protostellar clouds: initial stages of collapse ( abstract from the journal ). ... Shustov B.M., Wiebe D.S., Tutukov A.V. Evolution of disk galaxies and loss of heavy elements into the intracluster medium. ... ApJ (Letters), 1998, 503 , L71-L74 ( astro-ph/9806155 ). ...

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• Основные публикации Дмитрия Вибе

Next: Public Understanding of Science, Up: Technical Research Summaries Previous: New Approaches to Risk . ... Michael Smith has been analysing new infrared data collected from 11 PPN and PN by Chris Davis (Joint Astronomy Centre, Hawaii) to search for clues as to how the objects evolve. ... Georgi Pavlovski studied the properties of supersonic turbulence in molecular clouds and its effect on the molecular cloud properties and their chemical evolution. ...

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• Armagh Observatory
• Spinning Star Formation
• Highlights 1999

... The presence of solid­state emission bands is compared to other indicators of circumstellar material, such as Hff emission, optical variability and sub­mm continuum fluxes. ... However, a strong dependence on spectral type of the central star seems to be present: stars with spectral type earlier than B9 show either amorphous silicate in absorption or infrared spectra dominated by PAH emission, whereas more than 70% of the stars of later spectral type show silicate emission. ...

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• ESO - Research Area: PLANETS AND STAR FORMATION
• Mario van den Ancker
• ESO - Thesis Topic: Use of CO rotational vibrational absorption spectroscopy to

Photon Scattering: Basic Principle of Photon Scattering . Audio Narration is available . No Scattering: Photon Source and Detector . ... For optical photons, scattering goes as wavelength to the -4 power. In the case of blue photons compared to red photons, this means that blue photons are about 10 times more likely to get scattered than red photons. ... Watch the blue photons scatter away from the detector . ... Interstellar dust make stars appear redder than they really are . ...

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• Formation of the Galaxies

... November 22, 1996 . Fliers Around the Blue Snowball Nebula . ... But now yet another mystery has come to light: what created the fast-moving gas clouds that appear around planetary nebula ? Dubbed FLIERs for Fast Low-Ionization Emission Regions, these knots of dense gas appear to have been ejected from the central star before it cast of the planetary nebula. ... In the above false-color picture of NGC 7662, the Blue Snowball Planetary Nebula , the FLIERs are featured in the image inserts. ...

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• APOD: 2003 April 7 - NGC 281: Cluster, Clouds, and Globules
• APOD: 2004 October 20 - NGC 281: Cluster, Clouds, and Globules
• APOD: September 25, 1996 - Bright Stars and Dark Clouds

... For SIMS (Secondary Ion Mass Spectrometry) analysis, a solid surface is bombarded by primary ions of some keV energy. ... The subsequent mass analysis of the emitted ions provides detailed information on the elemental and molecular composition of the surface. ... Extremely short ion pulses with a duration below . ... By rastering a fine-focussed ion beam over the surface, like an electron beam in an electron microprobe, mass resolved secondary ion images (chemical maps) can be obtained...

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Astronomical Data Analysis Software and Systems XIII ASP Conference Series, Vol. ... A new Instrument module allows for plotting of the model points convolved with the spatial and spectral responses of the selected instrument. ... The model outputs are averaged over the instrument bands using the same weighting ( F = constant) as the SIRTF data pipeline which allows the SIRTF data products to be compared directly with the model database. ... The model the user has selected is highlighted (dark cubes). ...

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• ADASS 2003 Conference Proceedings
• Slitless Multiobject Spectroscopy with FOSC Type Instruments
• Near-IR Imaging of Star-forming Regions with IRAF

Main planetology and astrophysics scientific tasks of gamma-spectrometry GRS and detector HEND . ... The origin of Mars . The ratio of natural radioactive isotopes 19 K/ 92 U will allow to estimate the temperature of proto-planetary cloud in the point of Mars creation . ... Abundance of main elements at valleys and at plateaus will allow to determine their ages . ... Water as a factor of Mars global evolution, the presence of water and water ice under the surface in the present time . ...

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• Space Research Institute (IKI) Seminar
• Space Physics Group of Oulu
• Lagrangian Points

... SUN MOON MERCURY VENUS MARS, JUPITER SATURN . ... Mars . ... Spacecraft detects aurora and mysterious dust cloud around Mars . Although the source and composition of the dust are unknown, there is no hazard to MAVEN and other spacecraft orbiting Mars. ... MARS | ... NASA s Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft has observed two unexpected phenomena in the martian atmosphere: an unexplained high-altitude dust cloud and aurora that reaches deep into the martian atmosphere. ...

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• Is there evidence of Oort-Cloud-like structures around other stars? |
• Starless cloud cores reveal why some stars are bigger than others |
• Venus vortices go for chaotic multi-story strolls around the poles |

... We have measured this "redshift" for the pink black holes, and allowed for it in our calculations. ... We see this effect in the emission from gas around these pink black holes, but it is far too small an effect to account for the pinkness. Thus the swirling motions of gas around or into the black holes cannot produc the colour. ... At first we thought that these things were normal blue black holes hidden behind clouds of interstellar dust, that absorbed the blue light and made them appear pink. ...

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• Philip Lah's Research
• Dopita Papers
• Mike Bessell

... We present the fifth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). ... The data of this snap-shot spectroscopy survey confirmed 166 emission-line objects out of 209 observed candidates and allowed their quantitative spectral classification and redshift determination. ... For the remaining 30 previously known ELGs we give either improved data of the line intensities or some independent measurements. ... Galaxies ...

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• Optical spectroscopy
• Classification criteria
• cloud

... Posts tagged ?Differential Emission Measure? ... Differential Emission Measures (DEMs) are a summary of the temperature structure of the outer atmospheres (aka coronae) of stars, and are usually derived from a select subset of line fluxes. ... Continue reading ?Differential Emission Measure [Eqn]? Tags: DEM , Differential Emission Measure , EotW , Equation , Equation of the Week , stellar coronae . ... vlk on [MADS] Parallel Coordinates . upvc windows on [MADS] Parallel Coordinates . ...

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• The AstroStat Slog Blog Archive Differential Emission Measure [Eqn]
• Chandra Images for SNR J0535.7-6918
• Chandra Images for G039.7-02.0W

Next: Unusual Emission near a Up: NICMOS Science Previous: The Stellar Population in . ... Three examples are presented of how ISOCAM 1 sees the process of stellar evolution. i) Standard staring and coronographic observations with ISOCAM towards BD+31 643 are presented. ... Position 4 is closest to the star; Position 6 coincides roughly with the minimum of emission seen in the images; position 7 with the ring. ... I presented three examples of the evolution of stars as seen with ISOCAM. ...

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• stecf.slitless - a Slitless Spectroscopy Quick-look Tool
• Limits on the Star Formation Rates of z>2 Damped Ly Systems from H Spectroscopy
• NICMOS Science