2005A&A...442..469B


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET00:25:59

2005A&A...442..469B - Astronomy and Astrophysics, volume 442, 469-478 (2005/11-1)

XMM-Newton spectral properties of the ultraluminous IRAS galaxy Mrk 273.

BALESTRA I., BOLLER T., GALLO L., LUTZ D. and HESS S.

Abstract (from CDS):

We present a 23 ks XMM-Newton observation of the Ultraluminous Infrared Galaxy (ULIRG) Mrk 273. The hard X-ray spectrum can be modeled by a highly absorbed (∼7x1023cm–2) power law plus an Fe Kα emission line. The iron line (detected at more than 99% c.l.) is broad (σ=0.26+0.37–0.17keV), suggesting possible superposition of a neutral iron line at 6.4 keV, and a blend of ionized iron lines from Fe XXV and Fe XXVI. Given the relatively short exposure, the three line components cannot be individually resolved with high statistical significance: the neutral component is detected at ∼2.5σ and the Fe XXV line at ∼2σ c.l., while for the Fe XXVI line we can only estimate an upper limit. The broad band spectrum requires, in addition to a highly absorbed power law, at least three collisionally ionized plasma components, which may be associated with star-forming regions. The temperatures of the three plasmas are about 0.3, 0.8 and 6keV, where the highest of the three is sufficient to produce ionized iron emission lines. An alternative interpretation for the origin of the soft emission might also be reflection off photoionized gas, as has been observed in a number of nearby Compton-thick Seyfert 2 galaxies (e.g. NGC 1068, Circinus, Mrk 3, NGC 4945). A hot gas, photoionized by the primary, continuum can also produce ionized iron lines. Unfortunately, given the limited statistics and the lack of high resolution spectroscopy, it is not possible to distinguish between the two models investigated. We further compare the XMM-Newton findings with the Chandra data obtaining consistent spectral results. The absorption-corrected hard X-ray luminosity of Mrk 273 is L2–10keV∼7x1042erg/s, corresponding to ∼0.2% of the far-IR luminosity, similar to typical values found in pure starbursts. The thermal contribution to the soft X-ray luminosity is approximately 0.2-0.7x1042/ergs, comparable to those found in NGC 6240 and other starburst-dominated ULIRGs. We also analyze the XMM-Newton spectrum of Mrk 273x, an unabsorbed Seyfert 2 galaxy at redshift z=0.458, which lies in the field of view of Mrk 273.

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Journal keyword(s): galaxies: individual: Mrk 273 - galaxies: individual: Mrk 273x - galaxies: Seyfert - X-rays: galaxies

Simbad objects: 11

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Number of rows : 11

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 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3000 2
2 SN 1986J SN* 02 22 31.33 +42 19 56.4   18.4 18.4     SNII 308 1
3 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4178 2
4 Mrk 3 Sy2 06 15 36.458 +71 02 15.24 14.21 14.03 12.97     ~ 861 3
5 SN 1995J SN* 12 32 38.34 +63 53 09.2     16.5     SNII 18 1
6 NGC 4945 Sy2 13 05 27.279 -49 28 04.44   9.31 14.40 7.55   ~ 1301 2
7 Mrk 273 Sy2 13 44 42.164 +55 53 13.53   15.68 14.91     ~ 835 3
8 NAME Mrk 273x Sy2 13 44 47.5 +55 54 11     20.8     ~ 26 0
9 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 1037 2
10 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2727 4
11 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1510 2

    Equat.    Gal    SGal    Ecl

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2021.03.03-00:25:59

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