meeting 2023 08 01 n315 - JacobPilawa/TriaxSchwarzschild_wiki_5 GitHub Wiki

• 68.1 ± 2.5 Mpc from Jensen SBF
• Ngroup = 14 (so not isolated at all, and this is the brightest group member with M_K = -26.3)
• Slow rotator (lambda_e = 0.063)
• GMOS IFU PA: 42.0 from BOX N315_PA_NOTE.txt; Mitchell IFU PA: 42.4 from BOX
• Existing ALMA CO BH Measurement
• 309 total bins = 249 GMOS bins, 60 Mitchell bins

we had only just begun playing around with N315 and still sorting out the kinematics when we last left off since the central bins are contaminated by the dust lane in the center. we had been in the process of trying to get something reasonable from the central-most bins by iteratively masking various bins from the fit

• i think it would make sense to continue from pretty much a clean slate with N315's kinematics, especially if we are looking to incorporate dust more carefully in future versions of TriOS
• nonetheless, i have a few plots below showing the results of the masking process

also note, this is what my old notes said about our "masking" process -- essentially i was taking the unsymmetrized kinematics from pPXF, symmetrizing the kinematics as if the bad bins didn't exist, and then manually placing bins back in the places with the value at the -R/+R equivalent location:

• Start with the unsymmetrized kinematics
• Remove any mention of the kinematics or bins from the kindata.dat and the bins_gmos.dat files
• Symmetrize the kinematics (without the first few bins at +R)
• After symmetrizing, put the bins back in the original location, with kinematics equal to the equivalent value at -R. Specifically, I matched Bin 0 to Bin 1, Bin 18 to Bin 16, Bin 19 to Bin 5, Bin 21 to Bin 3, and bin 24 to bin 6