2009 v4, Aug. 26: added HST filters: ACS 606w, Nic2 polarization v3, May 7: downgraded an f90 statement to f77 to make it work with g77 compiler. 2008 0) fixed a big with the streamline hole--the code was doing a polynomial shape when streamline was specified. 1) updated instructions.txt a) to describe how to add in new filters, b) describe which dust files are associated with the Wood et al. (2002) model numbers. c) tips for running with no envelope, d) optimizing the grid, e) clarify flux and intensity units of SED and images, f) correction on albedo definition 2) updated dust files to *extrap.par, to correctly extrapolate to 3.6 mm. 3) fixed planck emission when there is a big inner hole 4) updated T-calculation for first absorption. 5) Changed Avall.dat to print out A(V) instead of Tau_V. Now Avall.dat, Av_thet.dat and A_v.dat all print out A(V). 6) The atmosphere file format has changed from the 2005 version of the code. This is compatible with the format you can download from the YSO grid and fitter website (www.astro.wisc.edu/protostars) 7) Reset some disk variables if disk mass is 0. prevents some needless propagating divide-by-zeros. 8) plot files: plotsedt. integrates total, stellar, thermal, direct flux to give luminosities of each. (useful for debris disk models where you want L_Ir/L_star). 9) works with g77, gfortran and ifort compilers. 10) changed filt_nu output to state FWHM of wavelength range of filter functions instead of Full-width (for images). 2007 Apr. 5 Changes from previous version of the code: 1) Fixed a bug in the 20070121 version that gives bogus results (no dust emission or scattering) if disk mass (MASSD) is set to 0. You'd know it if this happened. 2) A new input parameter, DTHRESH, sets the density threshold in the disk at which the grain model switches from the 'disk upper layers' to the 'disk midplane'. This was buried in the code before so now it's easier for the user to vary it. 3) added NAP, number of apertures as an input parameter, for easier comparison to the Robitaille et al. (2006) grid of models. 2007 Jan. 21 Changes from the previous version of the code: 1) There was a bug in the Sept. 15 version. The option to use a Planck function for the stellar atmosphere was not working. It was using the stellar atmosphere file. That has been fixed. 2) Some of the plotting files in the IDL directory have been tweaked (improved slightly). 2006 Sept. 15 This is the version of the code that was used to run our grid of 200,000 YSO models (Robitaille et al. 2006). You can rerun model to produce images or tweak parameters. The grid is available at http://carvan.astro.wisc.edu/protostars. Changes from the previous version of the code: 1. The output flux is now scaled to the luminosity of the source. That is, the spectra are in units of nu*Fnu= ergs/s. To compare to data from a source at distance d, just divide by 4*pi*d^2. 2. The program now tracks the last point of origin of the photon, defined as a stellar or thermally emitted photon (but not a scattered photon unless it gets absorbed and reemitted). So now you can plot up stellar vs disk vs envelope origin photons (see instructions.txt plotting programs). A few versions ago, I added options for plotting thermal, scattered and direct stellar photons. Both of these are very interesting, in my opinion. 2. Made warning messages an option so you don't have to see them if you don't want to (I turn them off unless I'm testing the code). This makes for much smaller log files. 3. Changed image and color-color plots to use the same filter functions as used in the grid of models (Robitaille et al. 2006). 4. Option to use planck function for star instead of stellar atmosphere file. 5. The format of the stellar atmosphere files has changed, as well as scaling. Only one file is supplied with the code. A stellar atmosphere browser will be available on the protostars website so you can download a file with any Tstar and log-g in the format used for our code and plot files. 6. The aperture (of the output flux) specification is different--you specify a min and max aperture and the program computes aperture sizes with an r^2 power law. Currently it uses 5 apertures, but this can be changed in the source code. The grid of models used 50 apertures, so if you want to recreate this, change nap in srcdust/tts.txt and recompile the code (make clean; make ttsre). 7. Some things in the input file are a little different as described in more detail in the instructions.txt file. There's an option to use either alpha parameter or accretion rate to specify disk accretion. The disk scale height can be specified as a scale height at the star or a factor to multiply the scale height calculated at the dust sublimation temperature. 8. Lots of new and improved IDL plotting routines. The image plotting routines are much easier to use and they convert the images to fits files for easier use with your own programs. I added some polarization plotting programs (polarization maps and polarized flux images). The 3-color image plotting programs can also be used to make 3-color polarized flux images (cool!). A new program plots the disk optical depth surface as seen by the origin (or the star in the point-source emission approximation which is okay beyond about 20 stellar radii). Another new program plots average angle of exit, to show how it is not always centered at the angle bin center. A program plots the grain model properties vs wavelength. 8. the instructions.txt file describes the format of several input and output files in case you want to supply your own input files or use your own plotting routines. 2005 Apr. 15 1. I just realized I forgot to include an important directory in the last (few?) distributions. Either no one is using this code or you aren't letting me know when there are problems. Note, this problem wouldn't affect users who installed over previous versions. 2. changed input for disk accretion parameters. Due to requests from some users, went back to specifying disk accretion rate rather than alpha disk viscosity parameter. 3. disk now handles more combinations of flaring and density exponents (finally did the math for certain combinations I was too lazy to account for before); specifically b-a=-2 and b-a=-1.5, a=1, 0.5. 4. added a couple of checks for erroneous input. program will stop if RMIND>RMAXD; will reset RMAX=RMAXD if RMAXD>RMAX. 2005 Feb. 28 1. I introduced a bug a few versions ago. If you set CRMINSUB='YES' it set RMINE=RMIND=1 (* Rsub) regardless of what you input. it is supposed to scale to Rsub. i.e., if you put RMINE=2, it is supposed to set it to twice the dust sublimation radius. It does that now. (sorry about that...). 2. modified trho3d.pro. 3. including a new plotting program written by Stefano Pezzuto. 4. modified instructions.txt a bit. 2004 November 25 1. deleted some arrays that aren't used in this version of the program. 2. forgot to include a couple of IDL plot programs in previous version (plotsede and plotsedte, which plot 'peeled' spectra). In the process of making these, I discovered an error in the direct stellar and scattered flux in the peeled spectrum (I doubt you've tried to plot this so don't worry). It's fixed and you can see the stellar direct and scattered flux in the plotsedte program. 3. Added a couple of new parameters for the magnetospheric accretion hot spot. I decided you probably need to have more control over this model. New variables are the fractional area of the stellar hotspot, and the disk magnetosphere co-rotation radius, rtrunc. 2004 September 26 Lots of changes to I/O and plotting. Added accretion shock luminosity. 1. Trimmed input parameters (mctherm.par) so it's easier to understand. This makes the program less flexible for you: There's no longer a stellar hot spot option or double cavity (which makes it possible to have a thicker wall). If you want these things back, let me know. See the instructions.txt file for the updated list of input parameters. 2. Updated most of the plotting routines. plotsed now modifies the model SED for foreground extinction (input Av). It's now a lot easier to plot temperature, density (etc) arrays (no more fortran programs). There's a new program, plotsedt that separates the spectrum into total, thermal, stellar direct, stellar scattered. See instructions.txt for more details. 3. Added accretion shock luminosity following Calvet & Gullbring (1998, ApJ, 509:802) for the most part. We let half the accretion luminosity (from the magnetospheric truncation radius, chosen to be 5 Rstar) go into x-rays, half into heating the stellar atmosphere. We use a grey solution (calculated by Jon Bjorkman) to calculate temperature of the heated atmosphere; i.e.,T=Tstar*(1+0.5*Lacc/Lstar/f)**0.2, where f is the ratio of shock area to star area. We use the median value of f=0.007 from Calvet & Gullbring. Our x-ray flux is emitted evenly from 100-500 A. We're not trying to model the x-ray spectrum yet, but need to include it since it heats the disk. In the future, we'll emit a Raymond-Smith spectrum. The heated atmosphere flux is emitted as a blackbody uniformly over the star. I don't think it matters much, but we can emit this from a ring or hot spots if you want. Let us know. 2004 June 18 1. new input variable CRMINSUB (see instructions.txt). if CRMINSUB='YES', program will scale RMIND,RMINE to the dust destruction radius. Otherwise, it scales to Rstar. The program calculates dust destruction radius based on an empirical fit (optically thin approximation is not accurate for the disk). 2. corrected calculated of stellar direct flux. wasn't normalizing properly. (affects dflux.dat, not flux.dat). 3. including a new variable tau_therm, in disk.dat. not sure I have it right yet so wait until next release. supposed to be an average optical depth of thermal photons. 2004 March 01 no new bugs. 1. changed the definition of EXF so density goes as rho=rhoconst*r^(-exf); previously went as r^exf. 2. changed description of EX1 and EX2 in input files.