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

Abstract

From a study of broad absorption line (BAL) + infrared (IR) + Fe ii 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 ([O ii], [Ne iii], [O iii], 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 + Fe ii QSOs – is discussed.

TWO-DIMENSIONAL MAPPING OF YOUNG STARS IN THE INNER 180 pc OF NGC 1068: CORRELATION WITH MOLECULAR GAS RING AND STELLAR KINEMATICS

“…This is the hypothesis put forth by Sakamoto et al (2006) to explain the presence of "superbubbles" observed in molecular gas emission in starburst galaxies such as NGC 253 and M 82 (Matsushita et al 2000). In the case of AGNs, the presence of superbubbles has been reported by Lipari and collaborators in a number of galaxies, examples being Mrk 231 (e.g., Lipari et al 2005 and references therein) and IRAS 04505-2958 (Lipari et al 2009). These authors suggest that broad absorption line (BAL) systems seen in the spectra of AGNs could be due to these superbubbles-giant expanding gas shells which originate in circumnuclear starbursts.…”

Cosmic Evolution of Size and Velocity Dispersion for Early-Type Galaxies

“…Such massive outflows (with ratesṀ out 1000M ⊙ yr −1 ) have been tentatively detected around quasars (e.g. Simcoe et al 2006;Prochaska & Hennawy 2009;Lípari et al 2009). D' Odorico et al (2004), studying narrow absorption line systems associated to six quasars, have shown that these outflows have chemical composition implying rapid enrichment on quite short timescales (see also Fechner & Richter 2009).…”

THE EXTRAORDINARY MID-INFRARED SPECTRAL PROPERTIES OF FeLoBAL QUASARS

“…Finding the youthful QSO population is a challenging and ongoing problem (e.g. Sanders et al 1988;Canalizo & Stockton 2001;Lacy 2006;Coppin et al 2008;Georgakakis et al 2009;Lípari et al 2009). Significant attention has focused on the Broad Absorption Line (BAL) QSOs (Lynds 1967;Weymann et al 1991;Brotherton et al 1998;Schmidt & Hines 1999;Arav et al 2001;Green et al 2001;Hall et al 2002;Reichard et al 2003;Priddey et al 2007;Gibson et al 2009), whose properties 10 have been explained either as arising from being observed at a particular orientation, or because they are young objects still partially surrounded by dust.…”