J/ApJ/779/87 MAGIICAT. III. Virial masses (Churchill+, 2013)
MAGIICAT.
III. Interpreting self-similarity of the circumgalactic medium with virial mass
using MgII absorption.
Churchill C.W., Trujillo-Gomez S., Nielsen N.M., Kacprzak G.G.
<Astrophys. J., 779, 87 (2013)>
=2013ApJ...779...87C 2013ApJ...779...87C
ADC_Keywords: Galaxy catalogs ; Equivalent widths ; Redshifts
Keywords: galaxies: halos; quasars: absorption lines
Abstract:
In Churchill et al. (2013ApJ...763L..42C 2013ApJ...763L..42C), we used halo abundance
matching applied to 182 galaxies in the MgII Absorber-Galaxy Catalog
(MAGIICAT) and showed that the mean MgIIλ2796 equivalent width
follows a tight inverse-square power law,
Wr(2796)∝(D/Rvir)-2, with projected location relative to
the galaxy virial radius and that the MgII absorption covering
fraction is effectively invariant with galaxy virial mass, Mh, over
the range 10.7≤logMh/M☉≤13.9. In this work, we explore
multivariate relationships between Wr(2796), virial mass, impact
parameter, virial radius, and the theoretical cooling radius that
further elucidate self-similarity in the cool/warm (T=104-104.5K)
circumgalactic medium (CGM) with virial mass. We show that virial mass
determines the extent and strength of the MgII absorbing gas such
that the mean Wr(2796) increases with virial mass at fixed distance
while decreasing with galactocentric distance for fixed virial mass.
The majority of the absorbing gas resides within D≃0.3Rvir,
independent of both virial mass and minimum absorption threshold;
inside this region, and perhaps also in the region 0.3<D/Rvir≤1,
the mean Wr(2796) is independent of virial mass. Contrary to
absorber-galaxy cross-correlation studies, we show there is no
anti-correlation between Wr(2796) and virial mass. We discuss how
simulations and theory constrained by observations support
self-similarity of the cool/warm CGM via the physics governing star
formation, gas-phase metal enrichment, recycling efficiency of
galactic scale winds, filament and merger accretion, and overdensity
of local environment as a function of virial mass.
Description:
Our sample comprises the 182 "isolated" galaxies in the "MgII
Absorber-Galaxy Catalog" (MAGIICAT; Nielsen et al. 2013, Paper I,
J/ApJ/776/114). Each galaxy has a published spectroscopic redshift. In
Table 1, we present the data employed for this work.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 149 182 Properties of the 182 "isolated" galaxies in
the "MgII Absorber-Galaxy Catalog"
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See also:
J/ApJ/776/114 : MAGIICAT. I. MgII absorber-galaxy catalog (Nielsen+, 2013)
J/ApJ/770/138 : Metallicities of Lyman limit systems and DLA (Lehner+, 2013)
J/ApJ/714/1521 : Spectroscopy of galaxies around distant QSOs (Chen+, 2010)
J/ApJ/698/819 : MgII and LRGs cross-correlation analysis (Lundgren+, 2009)
J/ApJ/660/1093 : Weak MgII absorbers at 0.4<z<2.4 (Narayanan+, 2007)
J/MNRAS/371/495 : Catalog of 1806 MgII absorbers from SDSS DR3 (Bouche+, 2006)
J/ApJ/559/654 : Lyα absorption systems. V. (Chen+, 2001)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Field Quasar Field identifier (HHMM+DDd; B1950 or
"SDSS")
10- 29 A20 --- JName Quasar J2000 identifier (JHHMMSS.ss+DDMMSS.s)
31- 36 F6.4 --- z [0.07/1.2] Galaxy spectroscopic redshift from
Paper I (Nielsen+, 2013, J/ApJ/776/114)
38- 42 F5.1 kpc D [5/194] Galaxy-quasar impact parameter
44- 48 F5.1 mag rMag [-24.2/-16.6] Absolute r band AB magnitude
50- 53 F4.1 [Msun] logM [10.7/13.9] Log of the virial mass
55- 57 F3.1 [Msun] e_logM [0.1/0.2] Lower uncertainty in logM
59- 61 F3.1 [Msun] E_logM [0.1/0.7] Upper uncertainty in logM
63- 65 I3 km/s Vmax [81/855] Maximum circular velocity (1)
67- 68 I2 km/s e_Vmax [11/59] Lower uncertainty in Vmax
70- 71 I2 km/s E_Vmax [30/64] Upper uncertainty in Vmax
73- 75 I3 kpc Rvir [69/845] Virial radius (1)
77- 78 I2 kpc e_Rvir [10/64] Lower uncertainty in Rvir
80- 81 I2 kpc E_Rvir [27/65] Upper uncertainty in Rvir
83- 86 F4.2 --- etav [0.02/1.6] ηV = D/Rvir (1)
88- 91 F4.2 --- e_etav [0/0.6] Lower uncertainty in etav (1)
93- 96 F4.2 --- E_etav [0/0.3] Upper uncertainty in etav (1)
98-100 I3 kpc Rc [3/175] Theoretical cooling radius (2)
102-103 I2 kpc e_Rc [0/18] Lower uncertainty in Rc (2)
105 I1 kpc E_Rc [2/7] Upper uncertainty in Rc (2)
107-111 F5.2 --- etac [0.03/19] ηC = D/Rc (1)
113-116 F4.2 --- e_etac [0/6.8] Lower uncertainty in etac (1)
118-121 F4.2 --- E_etac [0/10] Upper uncertainty in etac (1)
123-126 F4.2 --- Rc/Rv [0/2.6] Ratio Rc/Rvir (1)
128-131 F4.2 --- e_Rc/Rv [0/1.7] Lower uncertainty in Rc/Rv (1)
133-136 F4.2 --- E_Rc/Rv [0/0.5] Upper uncertainty in Rc/Rv (1)
138-142 F5.3 0.1nm Wr [0.003/4.5] MgII (2796Å) rest-frame
equivalent width in Å
144-149 F6.3 0.1nm e_Wr [0.001/0.3]?=-1 Uncertainty in Wr in Å
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Note (1): Uncertainties are based upon uncertainties in the virial masses. For
some quantities a larger (smaller) virial mass results in smaller
(larger) value such that the uncertainties anti-correlate.
Note (2): Because the slope of Rc changes sign as function of virial mass,
where the slope is positive the uncertainties correlate and where the
slope is negative they anti-correlate (see Figure B1). In the narrow
virial mass ranges where the slope of Rc changes sign, it is possible
that both the upward and downward uncertainties in virial mass can
result in an upward (or downward) uncertainty in Rc.
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History:
From electronic version of the journal
References:
Nielsen et al. Paper I. 2013ApJ...776..114N 2013ApJ...776..114N Cat. J/ApJ/776/114
Nielsen et al. Paper II. 2013ApJ...776..115N 2013ApJ...776..115N
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 29-Apr-2015