2009A&A...501...75A


Query : 2009A&A...501...75A

2009A&A...501...75A - Astronomy and Astrophysics, volume 501, 75-88 (2009/7-1)

The host in blue compact galaxies. Structural properties and scaling relations.

AMORIN R., ALFONSO J., AGUERRI J.A.L., MUNOZ-TUNON C. and CAIROS L.M.

Abstract (from CDS):

We characterise the underlying stellar host in a sample of 20 blue compact galaxies (BCGs), by fitting their two-dimensional light distributions. Their derived host structural parameters and those of eight other BCGs already obtained in a previous paper are related to galaxy properties, such as colours and gas content. These properties are also compared with those of other galaxy types. The structural parameters of the host were derived by fitting a two-dimensional PSF-convolved Sersic model to deep optical images in several bandpasses (B, V, R, I). We followed a fitting technique that consists in the accurate masking-out of the star-forming regions in several steps. All the BCG hosts but one show low Sersic indexes (0.5≲n ≲2), with mean effective radius <re,B≥1.11±0.74kpc and mean surface brightness <µe,B≥22.59±0.68mag/arcsec2. Host effective radii scale linearly with their luminosity, while n and µe do not. In addition, host colours and structural parameters are not linearly correlated. Overall, the flux enhancement caused by the starburst is about 0.8mag, while their B-R colours decrease by about 0.2mag. Galaxies with more luminous and extended hosts show larger and luminous starburst components, whereas the relative strength of the burst (Lburst/Lhost) does not show any significant dependence on the host luminosity (or mass). While hosts show B-R=0.95±0.26 in median, galaxies with redder hosts (<B-R≥1.29±0.10) and with bluer hosts (<B-R≥0.66±0.10) are distinguished among the more and less luminous systems, respectively. Overall, BCG hosts are more compact (by a factor ∼2) and have higher central surface brightnesses (by about ∼2mag) than dIs and most dEs. BCG hosts and isolated dIs are indistinguishable in the B-band Tully-Fisher relation (TFR). We found that about 50-60% of the galaxies are more underluminous than those late-type discs with the same circular velocity. This feature is more important when luminosities are converted into stellar masses, while it tends to diminish when the HI gas mass is added. Deviations among host masses for a given circular velocity from the stellar TFR correlate with their HI mass-to-luminosity ratio (MHI/LB), whereas deviations from the gas+stellar TFR do not. Overall, our findings suggest that the baryonic mass in BCGs tends to normal values, but BCGs tend to be inefficient by producing stars, especially toward the low-mass, gas-rich, and bluest hosts, in a similar way to dIs.

Abstract Copyright:

Journal keyword(s): galaxies: dwarf - galaxies: evolution - galaxies: fundamental parameters - galaxies: starburst - galaxies: structure - galaxies: photometry

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 Mrk 960 bCG 00 48 35.430 -12 42 59.77   15.5       ~ 105 0
2 6dFGS gJ012915.8-393037 H2G 01 29 15.865 -39 30 38.03   16.68   15.64   ~ 22 0
3 LEDA 8865 AG? 02 19 30.236 -00 59 06.46 17.71 18.15 17.57 17.44 17.35 ~ 30 0
4 NGC 1036 AG? 02 40 28.982 +19 17 49.48   13.5       ~ 117 0
5 Mrk 600 AG? 02 51 04.57 +04 27 13.9 14.76 15.07 14.70 14.50 14.29 ~ 123 0
6 LEDA 74944 EmG 03 42 49.4 -40 35 56 15.90 16.41 15.75 16.05 15.55 ~ 32 0
7 NGC 1741 EmG 05 01 38.3 -04 15 25   13.7   13.02 13.6 ~ 266 0
8 IC 399 EmG 05 01 44.0604445128 -04 17 19.319048052   15.0 14.8     ~ 71 0
9 Mrk 1094 bCG 05 10 48.1123757064 -02 40 53.685168744   14.0 14.4     ~ 89 1
10 UGCA 116 H2G 05 55 42.645 +03 23 32.23 10.74 11.68 11.46   11.82 ~ 538 0
11 Mrk 5 H2G 06 42 15.53 +75 37 32.6   17.0       ~ 111 0
12 NGC 2415 bCG 07 36 56.6678012232 +35 14 30.555503124   12.5       ~ 129 1
13 NGC 2537 AG? 08 13 14.643 +45 59 23.25 12.18 12.50 11.69 11.66   ~ 301 2
14 NGC 2893 AG? 09 30 16.9542533472 +29 32 23.895492828   13.6 13.11     ~ 125 1
15 Mrk 33 AG? 10 32 31.956 +54 24 03.53 13.29 13.66 13.13 12.71 12.27 ~ 368 1
16 NGC 3353 AGN 10 45 22.390 +55 57 37.36 12.90 13.25 12.79     ~ 359 1
17 Mrk 36 SBG 11 04 58.298 +29 08 16.54   15.5 15.29     ~ 225 0
18 Mrk 1307 Sy1 11 52 37.19 -02 28 09.9   14.79   14.09 14.9 ~ 172 0
19 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6660 0
20 Mrk 829 GiP 14 50 56.495 +35 34 18.27   14.5 14.83     ~ 209 0
21 UGC 9562 GiP 14 51 14.3956253136 +35 32 32.932212324   14.2       ~ 160 0
22 Mrk 487 bCG 15 37 04.237 +55 15 47.60   15.2       ~ 133 0
23 NGC 6052 AG? 16 05 12.8715178104 +20 32 32.607297132 13.01 13.44 13.00     ~ 352 2
24 PKS 2117+025 rG 21 20 28.52998462 +02 46 34.3083851   14.8       ~ 32 1
25 NAME Kinman Dwarf bCG 22 30 36.7959714600 -00 06 36.924915456 16.85 17.35 16.87   16.65 ~ 66 2
26 NGC 7468 bCG 23 02 59.172 +16 36 16.20   14.0       ~ 161 0
27 NGC 7518 GiP 23 13 12.7537321282 +06 19 18.411674658   14.5       ~ 98 0
28 NGC 7625 AG? 23 20 30.132 +17 13 32.16 13.31 13.23 11.98 11.25   ~ 264 0
29 Mrk 324 AG? 23 26 32.783 +18 16 00.07   15.5       ~ 66 0
30 LEDA 71605 EmG 23 30 09.7 +25 31 56   15.0       ~ 54 0

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