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Simulate spectroscopic observations of dwarf galaxies

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Simulate dwarf galaxies

This tool relies on the Ultra-faint Galaxy Likelihood (ugali) toolkit for simulating the spatial and color-magnitude distributions of stars in dwarf galaxies. Stellar velocities are simulated via a numerical integration of the Eddington formula.

Installation

Installation is not the easiest thing in the world, but you can check out the travis.yml.

Supported Instruments

  • DEIMOS on Keck
  • IMACS on Magellan
  • GIRAFFE on VLT
  • AAOmega/2dF on AAT
  • M2FS on Magellan
  • GMACS for GMT

Output Column Descriptions

The output of the dsphsim executable is an ascii table with the following columns.

Column Unit Description
RA deg Right ascension
DEC deg Declination
MAG_G mag DES g-band magnitude
MAG_I mag DES i-band magnitude
ANGSEP deg Angular separtion from dwarf centroid
RPROJ kpc Projected radial separation from dwarf centroid
SNR Simulated signal-to-noise ratio for spectroscopy
VTRUE km/s True simulated random velocity drawn from the underlying distribution
VSTAT km/s Adjustment to true velocity from statistical measurement uncertainty related to the brightness of each star.
VSYS km/s Adjustment to true velocity from instrumental systematic uncertainty
VMEAS km/s Velocity measured by instrument
VMEAS = VTRUE+VSTAT+VSYS
VMEASERR km/s Measured statistical velocity error
VSYSERR km/s Assumed instrumental systematic velocity error
VERR km/s Quadrature sum of VMEASERR and VSYSERR
VERR = sqrt(VMEASERR2+VSYSERR2)

The code used to generate these data products can be found in dsphsim/simulator.py.

This table can be read into a numpy array using numpy.genfromtxt:

import numpy as np
filename = "<your_filename.dat>"
data = np.genfromtxt(filename,names=True,dtype=None)

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Simulate spectroscopic observations of dwarf galaxies

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