2017A&A...608A..42K


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET02:06:16

2017A&A...608A..42K - Astronomy and Astrophysics, volume 608A, 42-42 (2017/12-1)

Comparative testing of dark matter models with 15 HSB and 15 LSB galaxies.

KUN E., KERESZTES Z., SIMKO A., SZUCS G. and GERGELY L.A.

Abstract (from CDS):

Context. We assemble a database of 15 high surface brightness (HSB) and 15 low surface brightness (LSB) galaxies, for which surface brightness density and spectroscopic rotation curve data are both available and representative for various morphologies. We use this dataset to test the Navarro-Frenk-White, the Einasto, and the pseudo-isothermal sphere dark matter models.
Aims. We investigate the compatibility of the pure baryonic model and baryonic plus one of the three dark matter models with observations on the assembled galaxy database. When a dark matter component improves the fit with the spectroscopic rotational curve, we rank the models according to the goodness of fit to the datasets.
Methods. We constructed the spatial luminosity density of the baryonic component based on the surface brightness profile of the galaxies. We estimated the mass-to-light (M/L) ratio of the stellar component through a previously proposed color-mass-to-light ratio relation (CMLR), which yields stellar masses independent of the photometric band. We assumed an axissymetric baryonic mass model with variable axis ratios together with one of the three dark matter models to provide the theoretical rotational velocity curves, and we compared them with the dataset. In a second attempt, we addressed the question whether the dark component could be replaced by a pure baryonic model with fitted M/L ratios, varied over ranges consistent with CMLR relations derived from the available stellar population models. We employed the Akaike information criterion to establish the performance of the best-fit models.
Results. For 7 galaxies (2 HSB and 5 LSB), neither model fits the dataset within the 1σ confidence level. For the other 23 cases, one of the models with dark matter explains the rotation curve data best. According to the Akaike information criterion, the pseudo-isothermal sphere emerges as most favored in 14 cases, followed by the Navarro-Frenk-White (6 cases) and the Einasto (3 cases) dark matter models. We find that the pure baryonic model with fitted M/L ratios falls within the 1σ confidence level for 10 HSB and 2 LSB galaxies, at the price of growing the M/Ls on average by a factor of two, but the fits are inferior compared to the best-fitting dark matter model.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: halos - galaxies: structure - dark matter - dark matter

Simbad objects: 31

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Number of rows : 31

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 UGC 128 LSB 00 13 50.93 +35 59 36.6   16.5       ~ 87 1
2 UGC 1230 LSB 01 45 32.251 +25 31 17.28   17       ~ 78 0
3 AGC 180072 LSB 08 09 32.6 +22 33 34           ~ 47 0
4 LSB F563-1 LSB 08 55 01.4 +19 45 06           ~ 63 0
5 NGC 3038 EmG 09 51 15.4615250115 -32 45 09.244118167   12.50 11.60 12.5 11.9 ~ 62 0
6 NGC 3223 EmG 10 21 35.076 -34 16 00.44   11.82 10.82 10.35 11.2 ~ 162 0
7 LSB F568-3 LSB 10 26 59 +22 13.6           ~ 74 0
8 UGC 5750 G 10 35 45.11 +20 59 24.7   17       ~ 67 0
9 NGC 3333 EmG 10 39 49.816 -36 02 10.24   13.91   12.65 13.3 ~ 44 0
10 NGC 3453 EmG 10 53 40.5126174049 -21 47 34.127630263   13.87   12.57   ~ 34 0
11 NGC 3463 EmG 10 55 13.3640650398 -26 08 26.902263658   13.78   12.39   ~ 47 0
12 ESO 215-39 GiG 11 17 04.215 -49 12 05.26   14.08   13.35   ~ 52 1
13 UGC 6614 LIN 11 39 14.8715231180 +17 08 37.195414914   14.8       ~ 128 0
14 ESO 322-76 GiG 12 46 41.990 -40 01 29.22   14.30   14.0 13.6 ~ 29 0
15 ESO 322-77 GiG 12 46 55.616 -41 29 48.20   14.57       ~ 26 0
16 NGC 4679 EmG 12 47 30.249 -39 34 15.03   13.32 11.90 12.20 12.8 ~ 70 0
17 ESO 323-25 GiG 12 52 39.012 -39 01 41.83   13.41 13.39 12.17 12.9 ~ 55 0
18 NAME HYA-CEN SUPERCL SCG 13 14 -33.3           ~ 130 0
19 ESO 383-2 G 13 28 37.8237678259 -37 34 23.508211862   14.40   13.46   ~ 36 0
20 IC 4298 G 13 36 34.717 -26 33 13.90   14.16   12.77   ~ 41 0
21 IC 4319 GiG 13 43 26.572 -29 48 12.66   14.35   12.79   ~ 54 0
22 ESO 383-88 GiG 13 49 33.468 -33 04 08.88   14.19   13.02   ~ 42 0
23 ESO 446-1 EmG 14 03 16.476 -31 20 53.12   14.24   13.59   ~ 42 0
24 VLSB F579-V01 LSB 14 32 48.1 +22 45 58           ~ 33 0
25 LEDA 86657 LSB 15 57 27.483 +20 39 59.12           ~ 90 0
26 UGC 10310 IG 16 16 17.9040378078 +47 02 43.158504118   14.9       ~ 129 0
27 LEDA 87309 LSB 17 03 56.1 +10 10 49           ~ 15 0
28 UGC 11454 G 19 31 33.669 +49 52 46.41   17       ~ 16 0
29 UGC 11616 G 20 41 13.440 +63 30 38.51   17       ~ 26 0
30 UGC 11748 GiG 21 27 39.734 +45 28 58.70   17       ~ 28 0
31 UGC 11819 G 21 49 10.7170765630 +41 56 53.546091624   17       ~ 20 0

    Equat.    Gal    SGal    Ecl

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2021.03.03-02:06:16

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