2008A&A...489...85T


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.16CEST10:21:34

2008A&A...489...85T - Astronomy and Astrophysics, volume 489, 85-100 (2008/10-1)

XMM-Newton X-ray and optical monitor far UV observations of NGC 7070A and ESO 2400100 shell galaxies.

TRINCHIERI G., RAMPAZZO R., CHIOSI C., GRUETZBAUCH R., MARINO A. and TANTALO R.

Abstract (from CDS):

Shell galaxies are considered to be the debris of recent accretion/merging episodes. Their high frequency in low density environments suggests that these episodes could drive the secular evolution of at least some fraction of the early-type galaxy population. We present XMM-Newton X-ray observations of two shell galaxies, NGC 7070A and ESO 2400100, and far UV observations obtained with the optical monitor for these and for an additional shell galaxy, NGC 474, for which we also have near and far UV data from GALEX. We attempt to gain insight into the overall evolution as traced by their star formation history and hot gas content. The X-ray and far UV data are used to derive their X-ray spatial and spectral characteristics and their UV luminosity profiles. We use ad hoc models developed to investigate the age of the most recent episode of star formation from the (UV - optical) colors and line strength indices. The X-ray spatial and spectral analysis show significant differences in the two objects. A low-luminosity nuclear source is the dominant component in NGC 7070A (logLX=41.7erg/s in the 2-10keV band). In ESO 2400100, the X-ray emission is due to a low temperature plasma with a contribution from the collective emission of individual sources. In the optical monitor image ESO 2400100 shows a double nucleus, one bluer than the other. This is probably due to a very recent star formation event in the northern nuclear region. The extension of the UV emission is consistent with the optical extent of all galaxies, at different degrees of significance in different filters. The presence of the double nucleus, corroborated by the (UV-optical) colors and line strength indices analysis, suggests that ESO 2400100 is accreting a faint companion. We explore the evolution in the X-ray luminosity during accretion processes with time. We discuss the link between the presence of gas and age, since gas is detected either before coalescence or several Gyr (>3) after.

Abstract Copyright:

Journal keyword(s): galaxies: elliptical and lenticular, cD - X-rays: galaxies - ultraviolet: galaxies - galaxies: evolution

Simbad objects: 17

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Number of rows : 17

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 470 GiP 01 19 44.845 +03 24 35.90 12.63 12.53 11.78     ~ 240 1
2 NGC 474 GiP 01 20 06.696 +03 24 54.97 12.75 12.37 11.51 11.42 10.56 ~ 306 1
3 NGC 1549 GiP 04 15 45.223 -55 35 32.50 11.22 10.48 9.79 9.08   ~ 220 1
4 NGC 1553 GiP 04 16 10.4711638537 -55 46 48.107262747 10.76 10.10 9.40 8.74   ~ 346 2
5 NGC 2434 GiG 07 34 51.1487209121 -69 17 03.008825858 12.82 12.50 11.26 10.84   ~ 172 1
6 NGC 2403 AGN 07 36 51.396 +65 36 09.17 9.31 8.84 8.38 8.19   ~ 1569 1
7 NGC 3256 IG 10 27 51.284 -43 54 13.55   11.83 11.33 10.62 11.9 ~ 730 2
8 M 105 LIN 10 47 49.600 +12 34 53.87   10.56 9.76 9.12 8.18 ~ 1362 0
9 NGC 3585 GiG 11 13 17.109 -26 45 17.96   10.64   9.22   ~ 251 0
10 NGC 4494 GiP 12 31 24.034 +25 46 29.93   10.55 9.74     ~ 443 0
11 NGC 5256 PaG 13 38 17.8 +48 16 41   14.1 13.42     ~ 390 2
12 NGC 5322 SyG 13 49 15.24 +60 11 25.8   11.3       ~ 375 2
13 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2617 4
14 2E 3737 Sy1 16 37 46.4976250637 +11 49 49.209457135   16.98 16.50     ~ 103 0
15 NGC 7070 GiG 21 30 25.342 -43 05 13.56   12.70 12.29 11.76 12.4 ~ 57 0
16 ESO 287-34 GiG 21 31 47.292 -42 50 51.55   13.01 12.39 11.54   ~ 53 0
17 ESO 240-10 GiG 23 37 44.414 -47 30 22.92   12.49   11.15   ~ 45 0

    Equat.    Gal    SGal    Ecl

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2019.10.16-10:21:34

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