caravan.astro.wisc.edu

Interpreting Spectral Energy Distributions from Young Stellar Objects

Interpreting Spectral Energy Distributions from Young Stellar Objects. Back to front page. After December 15th 2015. Users will no longer be able to interactively fit sources in the online SED fitting tool, although existing users will still be able to log in to access previous results. Users interested in fitting YSO SED models to observations after this date should consider using the command-line version of the SED fitting tool. After March 31st 2016. Want to be kept informed of updates? II - Fitting o...

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Interpreting Spectral Energy Distributions from Young Stellar Objects | caravan.astro.wisc.edu Reviews

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Interpreting Spectral Energy Distributions from Young Stellar Objects. Back to front page. After December 15th 2015. Users will no longer be able to interactively fit sources in the online SED fitting tool, although existing users will still be able to log in to access previous results. Users interested in fitting YSO SED models to observations after this date should consider using the command-line version of the SED fitting tool. After March 31st 2016. Want to be kept informed of updates? II - Fitting o...

<META> KEYWORDS

1 please note

2 welcome

3 protostars subscribe@googlegroups com

4 information

5 read this first

6 model sed browser

7 ascii files

8 let us know

9 sed fitting tool

10 general

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please note,welcome,protostars subscribe@googlegroups com,information,read this first,model sed browser,ascii files,let us know,sed fitting tool,general,radiation transfer codes,download bibtex entry,from ads

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Interpreting Spectral Energy Distributions from Young Stellar Objects | caravan.astro.wisc.edu Reviews

https://caravan.astro.wisc.edu

Interpreting Spectral Energy Distributions from Young Stellar Objects. Back to front page. After December 15th 2015. Users will no longer be able to interactively fit sources in the online SED fitting tool, although existing users will still be able to log in to access previous results. Users interested in fitting YSO SED models to observations after this date should consider using the command-line version of the SED fitting tool. After March 31st 2016. Want to be kept informed of updates? II - Fitting o...

INTERNAL PAGES

caravan.astro.wisc.edu

1

Model SED browser

http://caravan.astro.wisc.edu/protostars/grid.php

Back to front page. Enter numbers in decimal (e.g. 0.0002) or exponential (e.g. 1e-6) form. Select the range of parameters to search. A v [circumstellar] (mag). Disk Inner Radius (AU). Disk Inner Radius (Rsub). Disk Outer Radius (AU). Disk Scaleheight at 100AU. Disk accretion rate (Msol/yr). Envelope Accretion Rate (Msol/yr). Envelope Cavity Angle (degrees). Envelope Cavity density (cgs). Envelope Inner Radius (Rsub). Envelope Outer Radius (AU). A v [circumstellar] (mag). Disk Inner Radius (AU).

2

Radiation transfer code

http://caravan.astro.wisc.edu/protostars/codes.php

Back to front page. HO-CHUNK.ttsre.2008.tar.gz. Calculates radiative equilibrium temperature solution, thermal emission, scattering and polarization in 2-D protostellar geometries; good for computing spectral energy distributions (SEDs), polarization spectra, and images. Latest update: April 5th, 2007. The history of changes are listed here. This programs comes as a gzipped tar file - here's the easiest way to install:. If you have any problems installing or running the codes, don't hesitate to contact us.

3

Online SED Fitter - Home

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

Online SED Fitter - Home. Back to front page. Create an account here. Online YSO SED Fitting. Welcome to the online SED modeling tool. The method used by the online fitter to fit observed SEDs using the model SEDs from Paper I is described in Robitaille et al. (2007). If you are a new user, you can create an account here. If you already have a username and password, you can log in using the bar at the top of this page. Last Updated on 19th February 2016.

4

Information

http://caravan.astro.wisc.edu/protostars/info.php?topic=sedfitter

Back to front page. About the online SED fitting tool. The method is described in Robitaille et al (2007). And a discussion of some applications and limitations is given in Robitaille et al (2008). The results page should eventually come up. The main result will be a preliminary SED plot, and an ASCII file with the best 10,000 fits. You then have the option to create many different customized plots of the fits or parameters. Last Updated on 14th December 2010.

5

Information

http://caravan.astro.wisc.edu/protostars/info.php?topic=models

Back to front page. The model SEDs were computed using a Monte-Carlo radiation transfer code, for 20,071 different sets of physical parameters (e.g. stellar mass, disk mass, envelope infall rate, etc.), and for ten viewing angles, resulting in a total of 200,710 SEDs. The models are described in detail in Robitaille et al. (2006). Last Updated on 14th December 2010.

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gemelli.colorado.edu

Barbara Whitney

http://gemelli.colorado.edu/~bwhitney

Barbara A. Whitney. I am an astronomer working at the Space Science Institute. SSI) SSI is located in Boulder, CO, and I live and work in Madison, WI. I also work at the University of Wisconsin. Here's a picture illustrating my two main outdoor activities last winter (okay I can see this is out of date in the summer):. Bicycling and snow shoveling). Here's an artist's rendition of our Galaxy:. For more description and downloadable images. 10 viewing angles * 50 apertures = 10 million SEDs).

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SAGE: Surveying the Agents of a Galaxy's Evolution Team Profiles

http://sage.stsci.edu/team_N1.php

Principal Investigator: Margaret Meixner, STScI. Co-Investigator: Karl Gordon, STScI. Co-Investigator: Edward Churchwell, University of Wisconsin. Co-Investigator: Remy Indebetouw, University of Virginia. Co-Investigator: Joseph Hora, CFA/Harvard. Co-Investigator: Robert Blum, CTIO/NOAO. Co-Investigator: William Reach, IPAC/Caltech. Co-Investigator: Jean-Philippe Bernard, Centre d'Etude Spatiale des Rayonnements. Co-Investigator: Brian Babler, University of Wisconsin. Co-Investigator: Jay Frogel, AURA.

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Interpreting Spectral Energy Distributions from Young Stellar Objects

Interpreting Spectral Energy Distributions from Young Stellar Objects. Back to front page. After December 15th 2015. Users will no longer be able to interactively fit sources in the online SED fitting tool, although existing users will still be able to log in to access previous results. Users interested in fitting YSO SED models to observations after this date should consider using the command-line version of the SED fitting tool. After March 31st 2016. Want to be kept informed of updates? II - Fitting o...

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