J/MNRAS/445/3512 Surface density of dark matter haloes (Saburova+, 2014)
On the surface density of dark matter haloes.
Saburova A., del Popolo A.
<Mon. Not. R. Astron. Soc., 445, 3512-3524 (2014)>
=2014MNRAS.445.3512S 2014MNRAS.445.3512S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs
Keywords: galaxies: formation - galaxies: haloes
Abstract:
In this article, we test the conclusion of the universality of the
dark matter (DM) halo surface density µ0D=ρ0*r_0.
According to our study, the dispersion of values of µ0D is twice as
high as that found previously by other authors. We conclude that the
DM surface density and its Newtonian acceleration are not constant but
correlate with the luminosity, morphological type, (B-V)0 colour
index and content of neutral hydrogen. These DM parameters are higher
for more luminous systems of early types with red colour and low gas
content. We also found that the correlation of DM parameters with
colour index appears to be the manifestation of a stronger relation
between DM halo mass and the colour of a galaxy. This finding is in
agreement with cosmological simulations. These results leave little
room for the recently claimed universality of DM column density. We
also found that isolated galaxies in our sample (contained in the
Analysis of the interstellar Medium of Isolated GAlaxies (AMIGA)
catalogue) do not differ significantly in their value of µ0D from
the entire sample. Thus, since the AMIGA catalogue gives a sample of
galaxies that have not interacted with a significant mass neighbour in
the past 3Gyr, the difference between systems with low and high values
of µ0D is not related to merging events during this period of
time.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 105 211 The properties of sample galaxies
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Name of the galaxy
13- 18 F6.2 Mpc Dist Adopted distance
20- 24 A5 --- MType Morphological type taken from Hyperleda
database
27- 32 F6.2 mag BMAG ?=- Absolute B-band magnitude
34- 37 F4.2 [Msun/pc2] logmu0 logarithm of DM halo central surface
density
39- 42 F4.2 [Msun/pc2] E_logmu0 ? positive error of logmu0
44- 47 F4.2 [Msun/pc2] e_logmu0 ? negative error of logmu0
49- 53 F5.2 [cm/s2] loggDM logarithm of the DM Newtonian acceleration
at r0
55- 58 F4.2 [cm/s2] E_loggDM ? positive error of loggDM(r0)
60- 63 F4.2 [cm/s2] e_loggDM ? negative error of loggDM(r0)
65- 69 F5.2 [Msun] logMh(r25) logarithm of the DM halo mass inside the
optical radius
71- 74 F4.2 [Msun] E_logMh(r25) ? positive error of logMh(r25)
76- 79 F4.2 [Msun] e_logMh(r25) ? negative error of logMh(r25)
81- 95 A15 --- Ref Source of the DM halo parameters (1)
96-105 A10 --- Method Method of estimation of the DM
parameters (2)
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Note (1): Source of the DM halo parameters as follows:
1 = Athanassoula et al. (1987A&A...179...23A 1987A&A...179...23A)
2 = Barnes et al. (2004AJ....128.2724B 2004AJ....128.2724B)
3 = Begum & Chengalur (2004A&A...424..509B 2004A&A...424..509B)
4 = Chemin et al. (2006AJ....132.2527C 2006AJ....132.2527C)
5 = Corbelli (2003MNRAS.342..199C 2003MNRAS.342..199C)
6 = de Blok & Bosma (2002A&A...385..816D 2002A&A...385..816D, Cat. J/A+A/385/816)
7 = Cardone & Del Popolo (2012MNRAS.427.3176C 2012MNRAS.427.3176C)
8 = Lelli et al. (2010A&A...516A..11L 2010A&A...516A..11L)
9 = Humphrey et al. (2006ApJ...646..899H 2006ApJ...646..899H)
10 = Kasparova (2012AstL...38...63K 2012AstL...38...63K)
11 = Kuzio de Naray et al. (2008ApJ...676..920D 2008ApJ...676..920D)
12 = Frigerio Martins (2009, PhD thesis, SISSA)
13 = de Blok & McGaugh (1997MNRAS.290..533D 1997MNRAS.290..533D)
14 = Napolitano et al. (2009MNRAS.393..329N 2009MNRAS.393..329N, Cat. J/MNRAS/393/329)
15 = Napolitano et al. (2011MNRAS.411.2035N 2011MNRAS.411.2035N)
16 = Saburova & Zasov (2012AstL...38..139S 2012AstL...38..139S)
17 = Shchelkanova et al. (2013AstL...39..665S 2013AstL...39..665S)
18 = Spano et al. (2008MNRAS.383..297S 2008MNRAS.383..297S)
19 = Swaters et al. (2011ApJ...729..118S 2011ApJ...729..118S)
20 = Swaters et al. (2003ApJ...583..732S 2003ApJ...583..732S)
21 = de Blok et al. (2008AJ....136.2648D 2008AJ....136.2648D)
22 = van den Bosch & Swaters (2001MNRAS.325.1017V 2001MNRAS.325.1017V)
23 = van Eymeren et al. (2009A&A...505....1V 2009A&A...505....1V)
24 = Weijmans et al. (2008MNRAS.383.1343W 2008MNRAS.383.1343W)
25 = Weijmans et al. (2009MNRAS.398..561W 2009MNRAS.398..561W)
26 = Weldrake et al. (2003MNRAS.340...12W 2003MNRAS.340...12W)
27 = Wu (2007. preprint (0702233)
28 = Kasparova et al. (2014MNRAS.437.3072K 2014MNRAS.437.3072K)
Note (2): Method of estimation of the DM parameters as follows:
I = best fit model
II = maximum disk model
III = the method based on the stellar population synthesis model
color-mass-to-light ratio relation
IV = the approach based on the spectral energy distribution and
long-slit spectra modeling
V = the method relying on the marginal gravitational stability of the disk
VI = the approach taking into account the presence of spiral structure
VII = the method based on X-ray properties of hot gas
VIII = Jeans analysis based on planetary nebulae or stellar kinematical data
IX = the modeling reproducing the observed velocity dispersion profiles and
number density profiles
X = Bottema disk of de Blok & McGaugh (1997MNRAS.290..533D 1997MNRAS.290..533D)
For more details see paper.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 20-May-2015