Gemini GMOS IFU Spectroscopy of IRAS 04505-2958: A New Exploding BAL + IR + Fe II QSO
S. Lipari, M. Bergmann, S. Sanchez, R. Terlevich, Y. Taniguchi, E. Mediavilla, B. Punsly, B. Garcia, W. Zheng, D. Merlo
aa r X i v : . [ a s t r o - ph ] M a y Aso ia ión Argentina de AstronomíaBAAA, Vol. 50, 2007G. Dubner, M. Rovira and A. Piatti, eds.POSTER PAPERGemini GMOS IFU Spe tros opy of IRAS 04505-2958: ANew Exploding BAL + IR + Fe II QSOS. Lipari , M. Bergmann , S. San hez , R. Terlevi h , Y.Tanigu hi ,E.Mediavilla , B.Punsly, B.Gar ia , W.Zheng , D.Merlo Observatorio Astronomi o de Cordoba and CONICET; GeminiObservatory, Chile; Calar Alto Observatory, Spain; Univ. ofCambridge, UK; Tohoku Univ., Japan Inst. de Astrofísi a deCanarias, Spain; Johns Hopkins Univ., USA;Abstra t. New results of a Gemini GMOS Programme of study ofBAL+ IR+ Fe II QSOs are presented. We have performed a study ofthe kinemati s, morphologi al, and physi al onditions, in the BAL-QSO:IRAS 04505-2958. From this study, sele ted results are presented, mainlyfor the three more internal expanding shells. In parti ular, the GMOSdata suggest that the out(cid:29)ow pro esses (cid:21)in this QSO(cid:21) generated multipleexpanding hypergiant shells (from ∼
10, to ∼
100 kp ), in several extremeexplosive events. These new GMOS data are in good agreement with ourevolutionary, explosive and omposite model: where part of the ISM of thehost galaxy is eje ted in the form of multiple giant shells, mainly by HyNexplosions. This pro ess ould generate satellite/ ompanion galaxies, andeven ould expel a high fra tion (cid:21)or all(cid:21) the host galaxy. In addition, thisModel for AGN ould give important lues about the origin (cid:21)in AGNs(cid:21)of very energeti osmi rays, observed by the P. Auger ObservatoryResumen. Nuevos resultados de un programa Gemini GMOS de estu-dio de BAL + IR + Fe II QSOs son presentados. Nosotros estudiamosla morfologia, inemati a y ondi iones (cid:28)si as de IRAS 04505-2958. Re-sultados sele tos de este estudio se presentan en este trabajo, sobre 3 desus burbujas en expansion. Estos datos muestran un buen a uerdo onnuesto Modelo evolutivo, explosivo y ompuesto de AGNs/QSOs. Estemodelo explosivo de AGN podria darnos laves sobre el origen (cid:21)en AGN(cid:21)de los rayos osmi os dete tados por el Obsvatorio P. Auger.1. Introdu tion, The Programme, and ObservationsThere is in reasing eviden e that gala ti out(cid:29)ow (OF), broad absorption lines(BALs) and explosive events (ExE) play a main role, spe ially when the galaxiesand QSOs formed (see Lipari et al. 2007).1.1. Explosive BAL + IR + Fe II QSOs. The presen e of extreme explosionsand OF (cid:21)asso iated mostly to the end of extreme massive stars(cid:21) is an important omponent for di(cid:27)erent theoreti al models of galaxy/QSO evolution (see Lipariet al. 2007). From the observational point of view, the presen e of multiple1 on entri expanding supergiant bubbles/shells in young omposite BAL + IR+ Fe II QSOs, with entre in the nu leus and with highly symmetri ir ularshape ould be asso iated mainly with giant symmetri explosive events (Lípariet al 2003). These explosive events ould be explained in a omposite s enario:where the intera tion between the starburst and the AGN ould generate giantexplosive/HyperNova (HyN) events (see Collin & Zahn 1999).1.2. Evolutionary, Explosive and Composite Model for QSOs/AGNs.An evolutionary, explosive and omposite s enario was proposed for BAL + IR+ Fe ii QSOs (Lípari 1994, Lipari et al. 2005, Lipari & Terlevi h 2006). Wheremergers fuel extreme star formation pro esses and AGNs, resulting in strongdust and IR emission, large number of SN and HyN events, with expandingsuper giant bubbles/shells.1.3. IRAS 04505-2958. This IR sour e was asso iated with a luminous quasar(M V = (cid:21)25.8) at z = ′′ to the NW, from the nu leus)plus a possible tidal tail to the SE (at ∼ ′′ ). HST WFPC2 images show thatthe possible SE (cid:16)tail(cid:17) is a very omplex stru ture. Lipari et al. (2003) suggestedthat the SE tail/ring like stru ture is probably a large s ale (30 kp ) externalexpanding shell, at r ∼
11 kp . The BAL system in this IR QSO was dis overedby Lipari et al.(2005) based on the evolutionary IR olour- olour diagram (Fig.15 in their paper). Notably, the BAL shows the same blueshift as the main OF.1.5. Gemini GMOS-IFU and HST Observations. This study is basedon Gemini integral (cid:28)eld spe tros opy, ombined with Hubble Spa e Teles opeimages. 3D deep opti al spe tros opy of the nu lei and the 3 more internal ar sof IRAS 04505 − ′′ to the north-west; withoutother lear eviden e of the host galaxy. In the present GMOS study we foundthat this blob is omposite by 2 shells (S1 and S2) of r ∼ ′′ (1.1, 2.2 kp ).Shell S3: From a study of HST images + CASLEO spe tra of IRAS 04505 − ∼ ′′ ( ∼ α blobs at highredshift (Lipari & Terlevi h 2006).2.2. Gemini Results. Fig. 1a presents high resolution HST WFPC2 broad-band image/ ontours obtained in the opti al wavelengths through the (cid:28)lter WF2-F702W. This HST image shows: the QSO, the main on entri shell S3, and the(cid:28)eld G star. In addition, Figs. 1a shows the observed GMOS (cid:28)eld ( ∼
20 kp ×
28 kp ). The GMOS frame was entred lose to the middle position between theQSO and S3, at the PA ∼ o . Fig. 1b shows the [S ii℄/H α GMOS map.Figure 1. Left: HST WFPC2 Deep R Contour + GMOS (cid:28)eld.Rigth: [S ii℄/H α GMOS map.Shell S3: Fig. 1a shows the very extended morphology of the main super giantshell. This plot was performed using a s ale of (cid:29)uxes starting from very lowvalues. This very deep (cid:28)gure shows almost the omplete emission of S3, whi hshows highly symmetri and ir ular shape, with enter in the QSO.Here, we remark some interesting properties found using the GMOS-3D spe tra,the emission line and kinemati s maps: (i) all the GMOS (cid:28)eld (cid:21)in luding S3(cid:21)depi ts very extended emission line and also blue ontinuum (at s ale of ∼ αα