2009MNRAS.398..658L

Query : 2009MNRAS.398..658L

2009MNRAS.398..658L - Mon. Not. R. Astron. Soc., 398, 658-700 (2009/September-2)

Gemini 3D spectroscopy of BAL+IR+FeII QSOs - II. IRAS 04505-2958, an explosive QSO with hypershells and a new scenario for galaxy formation and galaxy end phase.

LIPARI S., BERGMANN M., SANCHEZ S.F., GARCIA-LORENZO B., TERLEVICH R., MEDIAVILLA E., TANIGUCHI Y., ZHENG W., PUNSLY B., AHUMADA A. and MERLO D.

Abstract (from CDS):

From a study of broad absorption line (BAL) + infrared (IR) + Feii quasi-stellar objects (QSOs) [using deep Gemini Multi-Object Spectrograph Integral Field Unit (GMOS-IFU) spectroscopy], new results are presented for IRAS 04505-2958. Specifically, we have studied in detail the outflow (OF) process at two large galactic scales: (i) two blobs/shells at radius r ∼ 1.1 and 2.2 kpc, and (ii) an external hypergiant shell at r ∼ 11 kpc. In addition, the presence of two very extended hypergiant shells at r ∼ 60-80 kpc is also discussed.

From this GMOS study the following main results were obtained. (i) For the external hypergiant shell, the kinematics GMOS maps of the ionized gas ([Oii], [Neiii], [Oiii], Hβ) show a small-scale bipolar OF, with similar properties to those observed in the prototype of exploding external supershells: NGC 5514. (ii) Three main knots - of this hypershell S3 - show the presence of a young starburst. (iii) The two internal shells show OF components with typical properties of nuclear shells. (iv) The two blobs and the hypershell are aligned at PA ∼ 131° showing bipolar OF shape at ∼10-15 kpc scale. In addition, the more external shells (at ∼60-80 kpc scale) are aligned at PA ∼ 40° also with bipolar OF shape (perpendicular to the more internal OF). (v) A strong blue continuum and multiple emission-line components were detected in all the GMOS fields.

The new GMOS data show a good agreement with an extreme + explosive OF scenario for IRAS 04505-2958, in which part of the interstellar medium (ISM) of the host galaxy was ejected (in multiple shells). This extreme OF could also be associated with two main processes in the evolution of QSOs: (i) the formation of companion/satellite galaxies by giant explosions; and (ii) to define the final mass of the host galaxy, and even if the explosive nuclear OF is extremely energetic, this process could disrupt an important fraction of the host galaxy. Finally, the generation of ultra-high-energy cosmic rays and neutrino/dark matter - associated with HyNe in explosive BAL + IR + Feii QSOs - is discussed.


Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS

Journal keyword(s): ISM: bubbles - galaxies: individual: IRAS 04505-2958 - quasars: absorption lines - galaxies: starburst

Simbad objects: 35

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Number of rows : 35
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 957 Sy1 00 41 53.4322147944 +40 21 17.647820820   15.94 15.14     ~ 103 0
2 Mrk 1502 Sy1 00 53 34.9331107632 +12 41 35.929269132   14.41 14.03     ~ 1168 1
3 IRAS 01003-2238 Sy2 01 02 49.9920152640 -22 21 57.262136544   18.62 18.9 17.83   ~ 164 0
4 2MASS J01395577+0619225 Sy1 01 39 55.7697705024 +06 19 22.520805888   16.80 17.00     ~ 178 0
5 SDSS J030000.56+004828.0 QSO 03 00 00.5687857104 +00 48 27.963948708   20.18 18.29     ~ 54 0
6 SN 2006gy SN* 03 17 27.06 +41 24 19.5       14.20   SNIIn 339 1
7 NGC 1260 GiG 03 17 27.2296053456 +41 24 18.481941324   14.2       ~ 93 1
8 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 940 1
9 LEDA 75249 Sy1 04 52 30.0811 -29 53 35.226 15.07 17.39 15.35 16.06   ~ 123 0
10 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SNIc: 548 0
11 IRAS 07598+6508 Sy1 08 04 30.4643108040 +64 59 52.789588188   14.3 15.5     ~ 231 0
12 NGC 2623 LIN 08 38 24.016 +25 45 16.29 14.10 13.99 13.36     ~ 498 1
13 QSO J0840+3633 QSO 08 40 44.4183146928 +36 33 27.831133836   17.51 16.98     ~ 67 0
14 SN 2008D SN* 09 09 30.625 +33 08 20.16     17.5     SNIb 405 1
15 NGC 3079 Sy2 10 01 57.8789863992 +55 40 47.449758324 11.57 11.54 10.86     ~ 1391 3
16 NGC 3256 Sy2 10 27 51.284 -43 54 13.55   11.83 11.33 10.62 11.9 ~ 848 2
17 QSO J1044+3656 QSO 10 44 59.6100662544 +36 56 05.153586864   17.27 16.94     ~ 73 0
18 * eta Car Em* 10 45 03.545808 -59 41 03.95124 6.37 7.03 6.48 6.123 4.41 LBV 2440 0
19 SDSS J114816.64+525150.3 QSO 11 48 16.647 +52 51 50.31   25.73 25.04     ~ 453 0
20 SN 2006tf SN* 12 46 15.81 +11 25 55.4     16.7     SNIIn 100 1
21 Mrk 231 Sy1 12 56 14.2341182928 +56 52 25.238373852   14.68 13.84     ~ 1988 3
22 SN 2005ap SN* 13 01 14.84 +27 43 31.4       18.20   SLSNIc 142 1
23 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4486 3
24 SN 1998E SN* 13 29 14.30 -33 10 38.0       16.5   SNIIn 7 1
25 LEDA 84105 Sy1 14 04 38.7980689872 +43 27 07.452879120   16.12 15.76     ~ 127 0
26 NGC 5514 AGN 14 13 38.690 +07 39 37.35   14.5       ~ 53 1
27 NVSS J143821+094623 QSO 14 38 21.3982504320 +09 46 23.182131612   21.25 20.36     ~ 17 0
28 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2961 4
29 Mrk 486 Sy1 15 36 38.4011947776 +54 33 33.215039244   15.21 14.78     ~ 275 0
30 Mrk 493 Sy1 15 59 09.6231720696 +35 01 47.561352852   15.69 15.06     ~ 310 0
31 IRAS 17002+5153 Sy1 17 01 24.8265469104 +51 49 20.447878836   15.49 15.12     ~ 385 0
32 Mrk 507 Sy1 17 48 38.423 +68 42 16.06   16.33 15.45     ~ 149 1
33 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1821 2
34 LEDA 66703 Sy1 21 24 41.6403183696 -17 44 45.886080696   17.18 16.50 15.95   ~ 92 0
35 NGC 7469 Sy1 23 03 15.6 +08 52 26 12.60 13.00 12.34     ~ 2096 3

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