User Tools

Site Tools

Trace:
tests:streams:challenges

Differences

This shows you the differences between two versions of the page.

Link to this comparison view

Both sides previous revisionPrevious revision
Next revision		Previous revision
tests:streams:challenges [2015/08/29 18:37] – cmateu_astrosen.unam.mxtests:streams:challenges [2022/10/24 12:26] (current) – external edit 127.0.0.1
Line 33: Line 33:
        * *.obs.* are convolved observable coordinates and error bars. The 11 columns are: apparent V magnitude, RA, dec, parallax, parallax error, proper motion in RA, PM_{RA} error, PM in dec, PM_{dec} error, RV, RV error.        * *.obs.* are convolved observable coordinates and error bars. The 11 columns are: apparent V magnitude, RA, dec, parallax, parallax error, proper motion in RA, PM_{RA} error, PM in dec, PM_{dec} error, RV, RV error.
   * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochrone.GaiaOnly.20streams.tgz|SphericalIsochrone.GaiaOnly.20streams.tgz]] --- subset of 20 streams convolved with Gaia errors, same naming convention/columns as above   * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochrone.GaiaOnly.20streams.tgz|SphericalIsochrone.GaiaOnly.20streams.tgz]] --- subset of 20 streams convolved with Gaia errors, same naming convention/columns as above
-  * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochone.GaiaOnly.subsample.tgz|SphericalIsochone.GaiaOnly.subsample.tgz]] --- for exploratory plotting purposes, two files containing 1/20th of the stars in each progenitor with full 6D coordinates, concatenated into one big list (~10MB), with (.cxv) and without (.txv) errors. +  * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochrone.GaiaOnly.subsample.tgz|SphericalIsochrone.GaiaOnly.subsample.tgz]] --- for exploratory plotting purposes, two files containing 1/20th of the stars in each progenitor with full 6D coordinates, concatenated into one big list (~10MB), with (.cxv) and without (.txv) errors. 
   * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochone.GaiaOnly.sub.info|SphericalIsochone.GaiaOnly.sub.info]] --- for each progenitor, lists the ID number, number of stars with full measured 6D positions (i.e. the number of rows in each of the data files in .All and .20streams), and number included in .subsample.   * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochone.GaiaOnly.sub.info|SphericalIsochone.GaiaOnly.sub.info]] --- for each progenitor, lists the ID number, number of stars with full measured 6D positions (i.e. the number of rows in each of the data files in .All and .20streams), and number included in .subsample.
   * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochrone.progs.info|SphericalIsochrone.progs.info]] --- information about the progenitors of the streams: ID#, *total* number of [RGB] stars in the original progenitor, time since infall in Myr, log luminosity in solar units, log *total* mass (stars+dark matter) in solar masses, scale radius in kpc, velocity dispersion in km/s, orbital apocenter radius in kpc, and orbital circularity [=L/L_circ(E)].   * [[http://user.astro.columbia.edu/~robyn/SphericalIsochrone.GaiaOnly/SphericalIsochrone.progs.info|SphericalIsochrone.progs.info]] --- information about the progenitors of the streams: ID#, *total* number of [RGB] stars in the original progenitor, time since infall in Myr, log luminosity in solar units, log *total* mass (stars+dark matter) in solar masses, scale radius in kpc, velocity dispersion in km/s, orbital apocenter radius in kpc, and orbital circularity [=L/L_circ(E)].
Line 159: Line 159:
  
   * $M_{Halo} = 1.81194\times 10^{12}\,M_{\odot}$   * $M_{Halo} = 1.81194\times 10^{12}\,M_{\odot}$
-  * $R_{Halo} = 32260\,pc$+  * $r_{Halo} = 32260\,pc$
   * $q_z = 0.8140$   * $q_z = 0.8140$
   * $M_{Pal5}(t=-4 Gyr) = 31090\,M_{\odot}$   * $M_{Pal5}(t=-4 Gyr) = 31090\,M_{\odot}$
   * $M_{Pal5}(t=today) = 13150\,M_{\odot}$   * $M_{Pal5}(t=today) = 13150\,M_{\odot}$
   * $d_{Sun} = 23190\,pc$   * $d_{Sun} = 23190\,pc$
-  * $V_C(R_{Sun}) = 249.01\,km/s$ +  * $V_C(r_{Sun}) = 249.01\,km/s$ 
-  * $V_C(R_{Pal5}) = 247.84\,km/s$ +  * $V_C(r_{Pal5}) = 247.84\,km/s$ 
-  * $V_C(R_{Halo}) = 251.99\,km/s$ +  * $V_C(r_{Halo}) = 251.99\,km/s$ 
-  * $a(R_{Sun}, 0, 0) = 7.95\,pc/Myr^2$ +  * $a(r_{Sun}, 0, 0) = 7.95\,pc/Myr^2$ 
-  * $a(R_{Pal5}) = a(7816 pc, 240 pc, 16640 pc) = 3.51\,pc/Myr^2$ +  * $a(r_{Pal5}) = a(7816 pc, 240 pc, 16640 pc) = 3.51\,pc/Myr^2$ 
-  * $a(R_{Halo}, 0, 0) = 2.06\,pc/Myr^2$+  * $a(r_{Halo}, 0, 0) = 2.06\,pc/Myr^2$
      
 == Functional form of the potential components == == Functional form of the potential components ==
Line 175: Line 175:
 Flattened NFW halo: Flattened NFW halo:
  
-  * $\Phi_{Halo}(R, z) = -\frac{GM}{\sqrt{R^2+\frac{z^2}{q_z^2}}}\ln\left(1+\frac{\sqrt{R^2+\frac{z^2}{q_z^2}}}{R_{Halo}} \right)$+  * $\Phi_{Halo}(R, z) = -\frac{GM}{\sqrt{R^2+\frac{z^2}{q_z^2}}}\ln\left(1+\frac{\sqrt{R^2+\frac{z^2}{q_z^2}}}{r_{Halo}} \right)$
  
 Jaffe bulge: Jaffe bulge:
  
-  * $\Phi_{Bulge} = \frac{GM_{Bulge}}{b_{bulge}}\ln{\frac{R}{R+b_{bulge}}$+  * $\Phi_{Bulge}(r) = \frac{GM_{Bulge}}{b_{bulge}}\ln{\frac{r}{r+b_{bulge}}$
   * $M_{Bulge} = 3.4\times 10^{10}\,M_\odot$   * $M_{Bulge} = 3.4\times 10^{10}\,M_\odot$
   * $b_{Bulge} = 700.0\,pc$   * $b_{Bulge} = 700.0\,pc$
Line 185: Line 185:
 Miyamoto-Nagai disk: Miyamoto-Nagai disk:
  
-  * $\Phi_{Disk} = -\frac{GM_{Disk}}{\sqrt{R^2+\left(a_{Disk}+\sqrt{z^2+b_{Disk}^2}\right)^2}}$+  * $\Phi_{Disk}(r) = -\frac{GM_{Disk}}{\sqrt{R^2+\left(a_{Disk}+\sqrt{z^2+b_{Disk}^2}\right)^2}}$
   * $M_{Disk} = 1.0\times 10^{11}\,M_{\odot}$   * $M_{Disk} = 1.0\times 10^{11}\,M_{\odot}$
   * $a_{Disk} = 6500\,pc$   * $a_{Disk} = 6500\,pc$
Line 258: Line 258:
 extracted from the Lowing et al. 2015 mock catalogues explained in the previous subsection. extracted from the Lowing et al. 2015 mock catalogues explained in the previous subsection.
  
-//Error prescriptions://  Proper motion and radial velocity errors have been simulated with Gaia error prescriptions as of Jun-2015 in [[ https://github.com/mromerog/Gaia-errors | Merce Romero’s Gaia error code]]. Photometric distance errors of 20% and 7% have been simulated for K giants and RR Lyrae stars respectively (these precisions are achievable using Gaia data for photometric distance measurements). The simulation of observables includes the effect of extinction, based on the 3D reddennig map from Drimmel et al. (2003). +//Error prescriptions://  Proper motion and radial velocity errors have been simulated with Gaia error prescriptions as of Jun-2015 in [[ https://github.com/mromerog/Gaia-errors | Merce Romero’s Gaia error code]]. Photometric distance errors of 20% and 7% have been simulated for K giants and RR Lyrae stars respectively (these precisions are achievable using Gaia data for photometric distance measurements). The simulation of observables includes the effect of extinction, based on the 3D reddennig map from Drimmel et al. (2003). The Sun has been placed at X=8 kpc with a velocity of (0,220,0)km/s.
  
 The SQL queries used to extract the stars are provided as part of each file’s header.  The SQL queries used to extract the stars are provided as part of each file’s header. 
Line 347: Line 347:
 Here are two mock catalogues for K giant stars in two Haloes from Andreea Font's LJMU Gas-Dynamical simulations (Font et al. in prep). We have used the same methods as for the [[#error-convolved_mock_catalogue_of_individual_halo_stellar_tracers|Error-convolved mock catalogue of individual halo stellar tracers]]: i.e. Ben Lowing's code (2015) to resample star particles into individual stars, Xue et al. (2014) criteria to select K giant stars and the same error prescriptions (described below). Here are two mock catalogues for K giant stars in two Haloes from Andreea Font's LJMU Gas-Dynamical simulations (Font et al. in prep). We have used the same methods as for the [[#error-convolved_mock_catalogue_of_individual_halo_stellar_tracers|Error-convolved mock catalogue of individual halo stellar tracers]]: i.e. Ben Lowing's code (2015) to resample star particles into individual stars, Xue et al. (2014) criteria to select K giant stars and the same error prescriptions (described below).
  
-//Error prescriptions://  Proper motion and radial velocity errors have been simulated with Gaia error prescriptions as of Jun-2015 in [[ https://github.com/mromerog/Gaia-errors | Merce Romero’s Gaia error code]]. Photometric distance errors of 20% have been simulated for K giants (e.g. Xue et al. 2014). The simulation of observables includes the effect of extinction, based on the 3D reddennig map from Drimmel et al. (2003). +//Error prescriptions://  Proper motion and radial velocity errors have been simulated with Gaia error prescriptions as of Jun-2015 in [[ https://github.com/mromerog/Gaia-errors | Merce Romero’s Gaia error code]]. Photometric distance errors of 20% have been simulated for K giants (e.g. Xue et al. 2014). The simulation of observables includes the effect of extinction, based on the 3D reddennig map from Drimmel et al. (2003). The Sun has been placed at X=8 kpc with a velocity of (0,220,0)km/s.
  
 The SQL queries used to extract the stars are provided as part of each file’s header.  The SQL queries used to extract the stars are provided as part of each file’s header. 
tests/streams/challenges.1440873448.txt.gz · Last modified: 2022/10/24 12:26 (external edit)