J/MNRAS/482/154 GHASP. spiral galaxies dark matter distribution (Korsaga+, 2019)
GHASP: an H α kinematics survey of spiral galaxies -
XII. Distribution of luminous and dark matter in spiral and irregular nearby
galaxies using Rc-band photometry.
Korsaga M., Amram P., Carignan C., Epinat B.
<Mon. Not. R. Astron. Soc., 482, 154-174 (2019)>
=2019MNRAS.482..154K 2019MNRAS.482..154K (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Models
Keywords: galaxies: dwarf - galaxies: haloes -
galaxies: kinematics and dynamics -
galaxies: spiral, dark matter
Abstract:
Mass models of 100 nearby spiral and irregular galaxies, covering
morphological types from Sa to Irr, are computed using Hα
rotation curves and Rc-band surface brightness profiles. The
kinematics was obtained using a scanning Fabry-Perot interferometer.
One of the aims is to compare our results with those from Korsaga et
al. 2018MNRAS.478...50K 2018MNRAS.478...50K, which used mid-infrared (MIR) WISE
(Wide-field Infrared Survey Explorer) W1 (3.4µm) photometric data.
For the analysis, the same tools were used for both bands.
Pseudo-isothermal (ISO) core and Navarro-Frenk-White (NFW) cuspy
models have been used. We test best-fitting models, maximum disc
models, and models for which mass-to-light ratio (M/L) is fixed using
the B-V colours. Similarly to what was found in the MIR 3.4µm band,
most of the observed rotation curves are better described by a central
core density profile (ISO) than a cuspy one (NFW) when using the
optical Rc band. In both bands, the dispersion in the (M/L) values
is smaller for the fixed M/L fits. As for the W1 photometry, the
derived dark matter halo' parameters depend on the morphological
types. We find similar relations than those in the literature, only
when we compare our results for the bulge-poor sub-sample because most
of previous results were mainly based on late-type spirals. Because
the dispersion in the model parameters is smaller and because stellar
masses are better defined in that band, MIR photometry should be
preferred, when possible, to the optical bands. It is shown that for
high-z galaxies, sensible results can still be obtained without full
profile decomposition.
Description:
We use a sample of 100 spiral and irregular nearby galaxies with
high-resolution Hα rotational curves (RCS), derived from 2D
velocity fields, and the optical Rc-band photometry: 73 from surface
brightness photometry obtained at the Observatoire de Haute Provence
(OHP) (Barbosa et al. 2015MNRAS.453.2965B 2015MNRAS.453.2965B, Cat. J/MNRAS/453/2965) and
27 from Sloan Digital Sky Survey (SDSS) DR7 (Abazajian et al.
2009ApJS..182..543A 2009ApJS..182..543A, Cat. II/294) archival data.
The RCs of this sample are selected from the GHASP survey, which
contains 203 galaxies observed with the 1.93m telescope of the OHP
using a Fabry-Perot interferometer scanning around the Hα
emission line with high spectral and spatial resolutions. The GHASP
data have been published in several previous papers(Garrido et al.
2002A&A...387..821G 2002A&A...387..821G, 2003A&A...399...51G 2003A&A...399...51G, 2005MNRAS.362..127G 2005MNRAS.362..127G;
Garrido, Marcelin & Amram 2004MNRAS.349..225G 2004MNRAS.349..225G; Epinat et al.
2008MNRAS.388..500E 2008MNRAS.388..500E, Cat. J/MNRAS/388/500, 2008MNRAS.390..466E 2008MNRAS.390..466E, Cat.
J/MNRAS/390/466).
First, we began with 124 galaxies, which have both Hα RCs and
optical Rc-band photometric data. Secondly, we assigned a quality
flag to the RC of each galaxy, ranging from 1 to 3: '1'for very high,
'2' for high, and '3' for low quality. To construct mass models with
good constraints, we therefore selected only galaxies with flag '1'
and '2' that reduced the sample to 100 galaxies. The 124 galaxies with
their global properties and quality flag are listed in Table A1.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 89 124 Global properties
tablea2.dat 119 100 Parameters of mass models using the BFM and
fixed M/L techniques with the pseudo-isothermal
(ISO) model
tablea3.dat 76 100 Parameters of mass models using the MDM
technique with the pseudo-isothermal (ISO) model
tablea4.dat 127 100 Parameters of mass models using the BFM and
fixed M/L techniques with the NFW model
--------------------------------------------------------------------------------
See also:
J/MNRAS/388/500 : GHASP: Hα data cubes for 108 galaxies
J/MNRAS/401/2113 : GHASP: Hα data cubes for 153 galaxies (Epinat+, 2010)
J/MNRAS/453/2965 : Surface photometry of GHASP galaxies (Barbosa+, 2015)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- ID Name of the galaxy in the UGC catalogue
(UGC NNNNN)
11 A1 --- f_B-V [*] * for galaxies with no B-V colour
available in the RC3 catalogue, the value
has been computed (1)
13- 24 A12 --- Type Morphological type taken from the RC3
catalogue (Third Reference Cat. of Bright
Galaxies (RC3)
de Vaucouleurs et al. 1991rc3..book.....D 1991rc3..book.....D,
Cat. VII/155) (2)
26- 29 F4.1 mag BMAG Absolute B magnitude from Epinat et al.
(2008MNRAS.388..500E 2008MNRAS.388..500E, Cat. J/MNRAS/388/500)
31- 34 F4.2 mag B-V (B-V) colours corrected for galactic and
internal extinction from RC3 catalogue
when available
36- 39 F4.1 mag/arcsec2 mu0obs Central surface brightness from the observed
data
41- 43 F3.1 --- R25/h Isophotal radius at the limiting surface
brightness of 25mag/arcsec2 normalized by
the disc scale length
45- 48 F4.1 --- Rlast/h The last radius of the RC normalized by the
disc scale length
50- 53 F4.1 mag/arcsec2 mu0 Central surface brightness of the disc
55- 57 F3.1 kpc h Disc scale length of the disc component
59- 64 F6.1 10+8Lsun LD Luminosity of the disc calculated at the
isophotal radius
66- 70 F5.2 mag/arcsec2 mue ? Surface brightness of the bulge at the
effective radius
72- 75 F4.2 kpc re ? Effective radius of the bulge
77- 80 F4.2 --- n ? Sersic index of the bulge
82- 87 F6.2 10+8Lsun LB ? Luminosity of the bulge derived at the
isophotal radius
89 I1 --- f_ID [1/3] Classification flag of the inner
galaxy rotation curves (RCs) (3)
--------------------------------------------------------------------------------
Note (1): Except for galaxies UGC 3521, 3708, 3915, 4393, 10652 for which the
morphological types are taken from Epinat et al. (2008MNRAS.388..500E 2008MNRAS.388..500E,
Cat. J/MNRAS/388/500)
Note (2): The colour corrected for extinction (B-V) was taken directly from the
RC3 catalogue for 62 galaxies of our sample and fitted for 38 galaxies
using the relation (B-V)=(-0.032±0.004)t+(0.73±0.02)
Note (3): Flag as follows:
1 = very high quality RCs
2 = high-quality RCs
3 = poor-quality RCs
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- ID Name of the galaxy in the UGC catalogue
(UGC NNNNN)
11 A1 --- f_ID [*] Flag on ID * : galaxies for which the
presence of dark matter is not necessary
13- 16 F4.2 Msun/Lsun M/LdBFM M/L of the disc from the best-fitting
model (BFM) for pseudo-isothermal (ISO)
core model (1)
18- 21 F4.2 Msun/Lsun E_M/LdBFM Upper error on M/LDBFM (1)
23- 26 F4.2 Msun/Lsun e_M/LdBFM Lower error on M/LDBFM (1)
28- 32 F5.2 Msun/Lsun M/LbBFM ? M/L of the bulge from the best-fitting
model (BFM) for pseudo-isothermal (ISO)
core model (1)
34- 37 F4.2 Msun/Lsun E_M/LbBFM ? Upper error on M/LBBFM (1)
39- 43 F5.2 Msun/Lsun e_M/LbBFM ? Lower error on M/LBBFM (1)
45 A1 --- l_r0BFM ? Lower limit flag on r0BFM (1)
47- 51 F5.1 kpc r0BFM Core radius of the dark matter halo from
the best-fitting model (BFM) for
pseudo-isothermal (ISO) core model (1)
53- 57 F5.1 kpc E_r0BFM ? Upper error on r0BFM (1)
59- 62 F4.1 kpc e_r0BFM ? Lower error on r0BFM (1)
64- 66 I3 10-3Msun/pc3 rho0BFM Central density of the dark matter halo
from the best-fitting model (BFM) for
pseudo-isothermal (ISO) core model (1)
68- 70 I3 10-3Msun/pc3 E_rho0BFM Upper error on rho0BFM (1)
72- 74 I3 10-3Msun/pc3 e_rho0BFM Lower error on rho0BFM (1)
76- 79 F4.1 --- Chi2BFM Reduced chi-squared from the best-fitting
model (BFM) for pseudo-isothermal (ISO)
core model (1)
81- 84 F4.2 Msun/Lsun M/LfML M/L derived using the B-V colour (2)
86- 89 F4.1 kpc r0fML Core radius of the dark matter halo from
pseudo-isothermal (ISO) core model with
fixed M/L (3)
91- 95 F5.1 kpc E_r0fML Upper error on r0fML (3)
97-100 F4.1 kpc e_r0fML Lower error on r0fML (3)
102-104 I3 10-3Msun/pc3 rho0fML Central density of the dark matter halo
from pseudo-isothermal (ISO) core model
with fixed M/L (3)
106-108 I3 10-3Msun/pc3 E_rho0fML Upper error on rho0fML (3)
110-112 I3 10-3Msun/pc3 e_rho0fML Lower error on rho0fML (3)
114-119 F6.1 --- Chi2fML Reduced chi-squared from
pseudo-isothermal (ISO) core model with
fixed M/L (3)
--------------------------------------------------------------------------------
Note (1): Values taken from the best fit for the pseudo-isothermal (ISO) core
model (Begeman 1987PhDT.......199B 1987PhDT.......199B)
Note (2): The relation between the M/L in the Rc band and the (B-V) colour
(Bell & de Jong 2001ApJ...550..212B 2001ApJ...550..212B) is given by
log(M/LR)=-0.660+1.222(B-V)
Note (3): Values taken from the pseudo-isothermal (ISO) core model fitting with
fixed M/L, derived from the (B-V) colour
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- ID Name of the galaxy in the UGC catalogue
(UGC NNNNN)
11- 15 F5.2 Msun/Lsun M/LdMDM M/L of the disc from the
pseudo-isothermal maximum disc model
(MDM) (1)
17- 20 F4.2 Msun/Lsun E_M/LdMDM Upper error on M/LdMDM (1)
22- 26 F5.2 Msun/Lsun e_M/LdMDM Lower error on M/LdMDM (1)
28- 32 F5.2 Msun/Lsun M/LbMDM ? M/L of the disc from the
pseudo-isothermal maximum disc model
(MDM) (1)
34- 38 F5.2 Msun/Lsun E_M/LbMDM ? Upper error on M/LbMDM (1)
40- 44 F5.2 Msun/Lsun e_M/LbMDM ? Lower error on M/LbMDM (1)
46- 49 F4.1 kpc r0MDM Core radius of the dark matter halo
from the pseudo-isothermal maximum disc
model (MDM) (1)
51- 54 F4.1 kpc E_r0MDM Upper error on r0MDM (1)
56- 59 F4.1 kpc e_r0MDM Lower error on r0MDM (1)
61- 63 I3 10-3Msun/pc3 rho0MDM Central density of the dark matter halo
from the pseudo-isothermal maximum disc
model (MDM) (1)
65- 67 I3 10-3Msun/pc3 E_rho0MDM Upper error on rho0MDM (1)
69- 71 I3 10-3Msun/pc3 e_rho0MDM Lower error on rho0MDM (1)
73- 76 F4.1 --- Chi2MDM Reduced chi-squared from the
pseudo-isothermal maximum disc model
(MDM) (1)
--------------------------------------------------------------------------------
Note (1): Values taken from the pseudo-isothermal maximum disc fit (MDM) that
minimizes the halo contribution by maximizing the stellar disc (and
bulge when present) contribution.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- ID Name of the galaxy in the UGC catalogue
(UGC NNNNN)
11- 14 F4.2 Msun/Lsun M/LdNFWBFM M/L of the disc from the best-fitting
model (BFM) for lambda-CDM cuspy
density profile (1)
16- 19 F4.2 Msun/Lsun E_M/LdNFWBFM Upper error on M/LdNFWBFM (1)
21- 24 F4.2 Msun/Lsun e_M/LdNFWBFM Lower error on M/LdNFWBFM (1)
26- 30 F5.2 Msun/Lsun M/LbNFWBFM ? M/L of the bulge from the best-fitting
model (BFM) for lambda-CDM cuspy
density profile (1)
32- 36 F5.2 Msun/Lsun E_M/LbNFWBFM ? Upper error on M/LbNFWBFM (1)
38- 42 F5.2 Msun/Lsun e_M/LbNFWBFM ? Lower error on M/LbNFWBFM (1)
44- 47 F4.1 --- cNFWBFM Central halo concentration index
from the best-fitting model (BFM) for
lambda-CDM cuspy density profile (1)
49- 52 F4.1 --- E_cNFWBFM Upper error on cNFWBFM (1)
54- 57 F4.1 --- e_cNFWBFM Lower error on cNFWBFM (1)
59- 63 F5.1 km/s VNFWBFM Halo velocity from the best-fitting
model (BFM) for lambda-CDM cuspy
density profile (1)
65- 69 F5.1 km/s E_VNFWBFM Upper error on VNFWBFM (1)
71- 75 F5.1 km/s e_VNFWBFM Lower error on VNFWBFM (1)
77- 80 F4.1 --- Chi2VNFWBFM Reduced chi-squared from the
best-fitting model (BFM) for
lambda-CDM cuspy density profile (1)
82- 85 F4.2 Msun/Lsun M/LNFWfML M/L derived using the B-V colour (2)
87- 91 F5.1 --- cNFWfML Central halo concentration index from
lambda-CDM cuspy density profile
fitting with fixed M/L (3)
93- 97 F5.1 --- E_cNFWfML Upper error on cNFWfML (3)
99-102 F4.1 --- e_cNFWfML Lower error on cNFWfML (3)
104-108 F5.1 km/s VNFWfML Halo velocity from lambda-CDM cuspy
density profile fitting with fixed
M/L (3)
110-114 F5.1 km/s E_VNFWfML Upper error on VNFWfML (3)
116-120 F5.1 km/s e_VNFWfML Lower error on VNFWfML (3)
122-127 F6.1 --- Chi2NFWfML Reduced chi-squared from lambda-CDM
cuspy density profile fitting with
fixed M/L (3)
--------------------------------------------------------------------------------
Note (1): Values taken from the best fit for the Navarro-Frenk-White (NFW)
lambda-CDM cuspy density profile model
(Navarro et al. 1996ApJ...462..563N 1996ApJ...462..563N)
Note (2): The relation between the M/L in the Rc band and the (B-V) colour
(Bell & de Jong 2001ApJ...550..212B 2001ApJ...550..212B) is given by
log(M/LR)=-0.660+1.222(B-V)
Note (3): Values taken from the Navarro-Frenk-White (NFW)
lambda-CDM cuspy density profile model with fixed M/L, derived from
the (B-V) colour
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Garrido et al., Paper I 2002A&A...387..821G 2002A&A...387..821G
Garrido et al., Paper II 2003A&A...399...51G 2003A&A...399...51G
Garrido et al., Paper III 2004MNRAS.349..225G 2004MNRAS.349..225G
Garrido et al., Paper IV 2005MNRAS.362..127G 2005MNRAS.362..127G
Spano et al., Paper V 2008MNRAS.383..297S 2008MNRAS.383..297S
Epinat et al., Paper VI 2008MNRAS.388..500E 2008MNRAS.388..500E, Cat. J/MNRAS/388/500
Epinat et al., Paper VII 2008MNRAS.390..466E 2008MNRAS.390..466E, Cat. J/MNRAS/390/466
Epinat et al., Paper VIII 2010MNRAS.401.2113E 2010MNRAS.401.2113E, Cat. J/MNRAS/401/2113
Torres-Flores et al., Paper IX 2011MNRAS.416.1936T 2011MNRAS.416.1936T
Barbosa et al., Paper X 2015MNRAS.453.2965B 2015MNRAS.453.2965B, Cat. J/MNRAS/453/2965
Korsaga et al., Paper XI 2018MNRAS.478...50K 2018MNRAS.478...50K
Korsaga et al., Paper XIII 2019MNRAS.490.2977K 2019MNRAS.490.2977K
(End) Ana Fiallos [CDS] 20-Jun-2022