meeting 2024 06 11 n777 - JacobPilawa/TriaxSchwarzschild_wiki_5 GitHub Wiki
- Summarizing the kinematic extraction, MGE fitting, and other input choices before running the first set of models.
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Stats:
- D = 68.0 ± 2.6, Jensen+21 SBF
- Brightest group member, 7 group members
- _e = 291 km/s
- Mk = -25.94, log10(Mstar) = 11.87
- eps = 0.17, lambda = 0.05 (Slow rotator)
- log10(Mhalo) = 13.5
- MASSIVE XIV: Note that MASSIVE XIV says this galaxy is aligned, whereas MASSIVE X says it is misaligned
- PA GMOS = 311 +/- 22
- PA Mitchell = 8 +/- 10
- PA Phot = 148.6 ± 0.8
- Psi GMOS = 18.1 ± 21.5 (MASSIVE XIV)
- Psi Mitchell = 39.6 (MASSIVE X)
- Photometry:
- has slightly increasing ellipticity with radius; the other parameters are all nearly constant.
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Recent paper from O'Sullivan which could be interesting!
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GMOS:
- All files seem to be on BOX.
- Has both symmetric and non-symmetric binning schemes.
- Other details:
- Files on BOX say:
- +X = 148 deg. E of N. in orbit modeling files
- +X = +X = -32 deg. E of N. in paperversion figures of kinematic moments
- PSF listed as: avg. FWHM = 0.39" (Gaussian)
- 128 bins (symmetric)
- 131 bins (non-symmetric)
- Files on BOX say:
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Mitchell
- All Mitchell files for all galaxies are present! There are folded and unfolded versions for everything. I'm currently sticking with our usual unfolded data.
- 64 bins (unfolded)
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First, I started by reproducing Irina's results:
- Symmetric binning scheme with the associated spectra located here: /Users/jacobpilawa/Research/N777/N0777/N777_spectra_20160603_voronoi_symmetric/
- Using the mask on BOX which has a different file name than the one listed by Irina below (doesn't seem to exist).
- Table 2 of Barth+02 for the template stars.
- Uncertainties are computed with 100 MC iterations.
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Irina lists the settings on BOX as:
Nominal settings for pPXF fits to NGC 777 GMOS data
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Wavelength range (rest): 8420-8730 A
Template list: barthlist.txt
(15 stars from Barth et al. 2002 -- spectra are from MILES Calcium Triplet library)
Spectrum mask: /GMOS/galaxy_files/N777/spectra/N777_spectra_mask1_nochipgap.fits
(bright sky lines as assessed from inspection of GMOS spectra)
(GMOS chip gap lies outside the pPXF wavelength range)
Initial velocity shift: 5000 km/s
Multiplicative polynomial: degree 3
Additive polynomial: degree 0 (constant offset)
Bias parameter: 0
- With these settings, I can get quite close to Irina's exact results. Here are some diagnostics from this reproduction.
- Note that the kinematics here are not point-symmetrized.
- These also use the symmetric binning scheme (whereas we'll likely use the non-symmetric binning scheme for the actual modeling), but I wanted to make sure I was able to reproduce her values.
| Bin Centers | Radial Moments | GMOS Maps | Mitchell Maps | Kinematic Comparison |
|---|---|---|---|---|
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And the spectra and resulting fits look beautiful!
| Plot |
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- Given that I can reproduce Irina's results more or less by fitting out to h6, I wanted to see how things change when fitting out to h8, so here are those diagnostics and comparisons to Irina.
- Note the settings from above are exactly the same; the only different is the cutoff of the GH series.
| Radial Moments | GMOS Maps | Mitchell Maps | Kinematic Comparison |
|---|---|---|---|
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Spectral fits out to h8
| Plot |
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- And lastly, here's what we'll likely use for the modeling. Note that this uses the non-symmetric binning scheme (so it's hard to compare directly to Irina's which is symmetrically binned).
| Bin Centers | Radial Moments | GMOS Maps | Mitchell Maps |
|---|---|---|---|
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Spectral fits out to h8 for the 131 asymmetric bins
| Plot |
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- Note these are the point-symmetrized versions of the kinematics.
| Sym vs. Non-Sym Comparison | Radial Moments | GMOS Maps | Mitchell Maps |
|---|---|---|---|
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- Started doing some preliminary MGE fitting and background information gathering for N410 while we try to track down the spectra.
- I've done our usual MGE fitting (unregularized) for a few different bounds on sigma (0,1,2,3,4) pixels from the center:
- I likely need to go back and regularize these given the distribution of some of the q' values (reaching sometimes ~0.4 or so, severely limit deprojection).
- The MGEs look alright, but I think there is some work that can be done. There seems to be a lot of contaminating light in the original image (see below), but we already are applying a mask, so unsure what to do beyond that.
- Note that the PA returned is 9.3 deg Left of Up. Need to correct for HST angle.
- This converts to a PA of -31.3 deg E of N (or +148.6 deg E of N)
| HST Image |
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| Comparing Deprojected 3D |
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| Plot | 0p0 | 1p0 | 2p0 | 3p0 | 4p0 |
|---|---|---|---|---|---|
| Large Scale Residuals |  |
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| Zoomed in Residuals |  |
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| Large Contours |  |
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| Zoomed Contours |  |
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| Major Axis vs. Points |  |
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| Deprojected |  |
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| Enclosed Light |  |
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And here are all of the components listed for each of these MGEs:
- 0p0:
I [Lsun/pc^2] Sig [arcsec] q PA
6813.27 0.0883087 0.923946 0
6362.68 0.292563 0.951884 0
9187.29 0.476592 0.981002 0
7434.14 0.791955 0.838695 0
8170.31 1.42443 0.852063 0
2735.83 2.61953 0.825411 0
1909.59 3.92614 0.850293 0
1115.52 6.50793 0.840326 0
181.839 10.6348 0.741224 0
326.649 15.9419 0.835402 0
103.238 27.5027 0.871661 0
24.3176 69.9949 0.680238 0
- 1p0:
I [Lsun/pc^2] Sig [arcsec] q PA
6675.26 0.1 0.843808 0
6417.88 0.300018 0.959512 0
8834.9 0.478646 0.980615 0
7478.61 0.788519 0.839527 0
8192.08 1.42327 0.851904 0
2742.99 2.61935 0.825517 0
1907.98 3.92872 0.850349 0
1115.2 6.51272 0.840147 0
181.151 10.6646 0.741096 0
326.351 15.9529 0.835706 0
103.026 27.5719 0.871323 0
24.0676 70.4358 0.678407 0
- 2p0:
I [Lsun/pc^2] Sig [arcsec] q PA
7490.47 0.2 0.737085 0
11040 0.42029 1 0
8624.08 0.763005 0.848944 0
8251.22 1.42119 0.851218 0
2743.55 2.61604 0.825884 0
1911.21 3.9245 0.850152 0
1117.18 6.50595 0.840267 0
182.282 10.6481 0.741553 0
326.369 15.9504 0.835601 0
103.095 27.5523 0.871401 0
24.1359 70.3143 0.678935 0
- 3p0:
I [Lsun/pc^2] Sig [arcsec] q PA
11789.7 0.3 0.876765 0
8162.93 0.549274 1 0
6063.63 0.837696 0.807172 0
8023.26 1.449 0.852578 0
2681.16 2.68425 0.824485 0
1818.03 3.95939 0.85205 0
1109.55 6.5217 0.839517 0
178.66 10.641 0.741297 0
326.499 15.9093 0.835023 0
104.018 27.3361 0.871914 0
24.8827 69.0207 0.68495 0
- 4p0:
I [Lsun/pc^2] Sig [arcsec] q PA
17244.4 0.4 0.909954 0
9261.93 0.898056 0.870633 0
6585.2 1.58343 0.843116 0
2438.83 2.84456 0.826855 0
1620.6 4.0191 0.853622 0
1106.37 6.53141 0.839053 0
178.372 10.7104 0.741393 0
325.567 15.9506 0.835736 0
103.138 27.5226 0.871406 0
24.2659 70.0647 0.680161 0
- Here are all the input files used in the modeling and the various choices I've made:
aperture_gmos/aperture_mitchell.dat
- The only real number that I control in these files are the
kin*gridthetavalues, which represent the difference between the MGE +x axis and the +x axis of the kinematics. - These numbers are computed as PA_MGE - PA_kinematics:
- The MGE PA comes from the fits abiove, which uses -31.3 (148.6) E of N
- The kinematic PAs come from the files on BOX.
- For GMOS, these values are listed in /MASSIVE/GMOS_kinematics/N0777/N0777_PA_note.txt, which lists the +x axis of the orbit modeling files as +148 deg E of N.
- For Mitchell, the numbers are located in /MASSIVE/Mitchell_reduced_data/NGC0777/kinematics_paperversion/unfolded/more_files/NGC0777-s2-unfolded-bininfo.txt, which lists the gal pa as +148.4 deg E of N.
- This means that the input files should have
kin1gridthetaandkin2gridthetaas 0.6 and 0.4, respectively.
bins_gmos/bins_mitchell.dat
- I don't make any choices for these files. These are generated when preparing the orbit model files and associated the apertures with specific kinematics.
kindata.dat
- This is our normal kindata.dat file, which comes from the Gh8Mh6 minimization described above.
- This file contains 12 moments total, 8 of which are measured for the GMOS data and are from my own spectral fits, and 6 moments are fit for Mitchell (which I obtained from the files on BOX).
- I've currently left in all bins, but we can decide to mask the overlapping Mitchell bins if we'd like.
- I've added dummy moments for GMOS h9 through h12 and Mitchell h7 through h12 by assigning all the values to 0.0, and uncertainties identical to the h7/h8 errors for GMOS and h5/h6 errors for Mitchell.
mge.dat
- Currently a placeholder MGE so that we can discuss the fits above.
orbitstart_loop/box.dat
- These are just auxillary files which point to other files in our models. No changes or choices.
orblib_loop/box.in
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The only specific changes I had to make here relate to the PSFs we assumed for each dataset:
- I obtained the PSF for GMOS from the file /MASSIVE/GMOS_kinematics/N0777/N777_GMOS_PSF.txt, which says that the average weighted PSF = 0.39". The code accepts the equivalent "sigma" for this PSF, which I obtain as sigma = 0.38/(2sqrt(2ln(2))) = 0.166.
- I am using the same PSF for Mitchell as we have used for the other galaxies, which has a sigma = 0.5, which is equivalent to a 1.177" PSF.
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Other notable parameters that I kept constant from past orbit modeling:
- innermost mass bin starts at 0.1"
- outermost mass bin starts at 100" and extends to 316"
- 200 dynamical time integration for the box library; 2000 dynamical times for the loop library
parameters_loop/box.in
- Many of these parameters are changed on the fly (mass components and angles).
- I'm using:
- nEner = 40 for both
- nI2 = 18, 9 for the loop and box library respectively
- nI3 = 9, 9 for both
- logrmin = 10^-2 arcsec (minimum IC radius in arcsec)
- logrmin = 10^2.5 arcsec (maximum IC radius in arcsec)
- interplogmin = 10^-8
- interplogmax = 10^2.6
- gnfw halo with gamma = 0
triaxmass.in
- Auxillary file which points to other files.
triaxmassbin.in
- Auxillary file which points to other files.
- Also contains the same PSF information present in orblib_loop/box.dat.
triaxnnls.in
- Mostly points to other files.
- I've ensured that this file correctly assumes we have 12 total moments.
- I've also checked to make sure that this file reads in both the loop orbit library and box orbit library.