The Host Galaxies of<i>IRAS</i>‐selected Quasi‐stellar Objects

Boyce, P. J.; Disney, M. J.; Blades, J. C.; Boksenberg, A.; Crane, P.; Deharveng, J. M.; Macchetto, F.; Mackay, Craig D.; Sparks, W. B.

doi:10.1086/178187

Cited by 51 publications

(62 citation statements)

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“…The PG 1700]518 system shows a marked similarity to the IRAS-discovered infrared-luminous QSO IRAS 04505[2958 (Low et al 1988), which itself consists of a QSO, a host galaxy, and a ringlike companion (Boyce et al 1996). The total non-QSO light in the PG 1700]518 system D4L * is comparable to that obtained for IRAS 04505[2958 (6L * ; Boyce et al 1996).…”

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confidence: 52%

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The Host Galaxy of the Broad Absorption Line QSO PG 1700+518 and Its Ring Galaxy Companion: NICMOS 1.6 Micron Imaging

Hines

Low

Thompson

et al. 1999

ApJ

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The 1.6 km Near Infrared Camera and Multiobject Spectrometer image of the broad absorption line QSO PG 1700]518 clearly resolves the QSO host galaxy and a ringlike companion. The companion is most likely a ring galaxy produced in a collision with the QSO galaxy D5 ] 107 yr ago. The morphology of the PG 1700]518 system is very similar to IRAS 04505 [2958[ (Boyce et al. 1996. Both objects were identiÐed in a sample of eight QSOs selected by "" warm ÏÏ far-IR colors and extreme IR luminosities (Low et al. 1988). All eight QSOs show signs of strong interaction, and the presence of two head-on colliding systems in this sample may suggest that small impact parameters favor the energizing of IRluminous QSOs. Subject headings : galaxies : peculiar È infrared : galaxies È quasars : individual (PG 1700]518)PG 1700]518 is one of the most infrared- Low et al. 1988Low et al. , 1989. It was originally identiÐed in the Palomar-Green Survey (Schmidt & Green 1983) and subsequently found to be one of only B2% of QSOs that show broad absorption lines (BALs) from low-ionization species such as Al III j1860 and Mg II j2800 (Wampler 1985 ;Pettini & Boksenberg 1985 ;Turnshek et al. 1985). Its IR luminosity, warm far-IR colors indicative of dust heated by a QSO UV continuum km) ¹ 3 : 60 Low et al. 198860 Low et al. , 1989, and its polarization properties Schmidt & Hines 1999 ;Schmidt, Hines, & Smith 1997), all suggest a strong connection with the ultra-and hyperluminous infrared galaxies (Sanders et al. 1988a ;Cutri et al. 1994 ;Hines et al. 1995).Previous ground-based optical and near-IR images of PG 1700]518 reveal a slight extension southwest and an arclike feature northeast of the bright point source B2A .5 (Hickson & Hutchings 1987 ;Hutchings, Ne †, & Gower 1992 ;Stickel et al. 1995). The "" E ] A ÏÏ optical spectrum of the arc implies an old population of stars plus an 85 Myr old starburst (Canalizo & Stockton 1997 ;Stockton, Canalizo, & Close 1998), and the small velocity o †set between the arc and the QSO (140 km s~1) suggests that the two are physically associated. Recent ground-based images using adaptive optics have shown that the arc is a discrete companion galaxy (Stockton et al. 1998), but the detailed morphology of this structure is still difficult to determine from ground-based images. In this contribution we present a deep 1.6 km image obtained with the Near Infrared Camera and Multiobject Spectrometer (NICMOS) aboard the Hubble Space T elescope (HST ). In the next section we present details of our observations and data reductions that may be useful to other NICMOS programs. We present the observed properties of the companion and QSO host galaxy in°3, and we then brieÑy discuss the signiÐcance of these results for understanding the connection between ultra-and hyperluminous infrared galaxies and QSOs. OBSERVATIONSPG 1700]518 was observed on UT 1997 October 28 through the F160W Ðlter of NICMOS camera 2 (NIC2). A four-position spiral-dither pattern with 50.5 pixel o †sets in the detector coordinate system was...

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confidence: 52%

“…The companion is most likely a ring galaxy produced in a collision with the QSO galaxy D5 ] 107 yr ago. The morphology of the PG 1700]518 system is very similar to IRAS 04505 [2958[ (Boyce et al 1996. Both objects were identiÐed in a sample of eight QSOs selected by "" warm ÏÏ far-IR colors and extreme IR luminosities (Low et al 1988).…”

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confidence: 99%

The Host Galaxy of the Broad Absorption Line QSO PG 1700+518 and Its Ring Galaxy Companion: NICMOS 1.6 Micron Imaging

Hines

Low

Thompson

et al. 1999

ApJ

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“…The HST image in the R band is strongly suggestive of a merger between two galaxies in its latest stage, according to Boyce et al (1996). They also noted that, given its low nuclear luminosity, it should be strictly classified as a Seyfert 1, instead of a QSO, but its colors clearly points toward a very large obscuration, so that it is very likely that it hosts a buried QSO.…”

Section: A Misclassified Compton-thick Object: Iras 13218+0552mentioning

confidence: 99%

A search for changing-look AGN in the Grossan catalog

Bianchi¹,

Guainazzi²,

Matt

et al. 2005

A&A

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We observed with XMM-Newton 4 objects selected from the Grossan (1992, Ph.D. Thesis) catalog, with the aim to search for new "changinglook" AGN. The sample includes all the sources which showed in subsequent observations a flux much lower than the one measured with HEAO A-1: NGC 7674, NGC 4968, IRAS 13218+0552 and NGC 1667. None of the sources was caught in a high flux state during the XMMNewton observations, whose analysis reveal they are all likely Compton-thick objects. We suggest that, for all the sources, potential problems with the HEAO A-1 source identification and flux measurement prevent us from being certain that the HEAO A-1 data represent a putative "high" state for these objects. Nonetheless, based on the high flux state and Compton-thin spectrum of its GINGA observation, NGC 7674 represents probably the sixth known case of a "changing-look" Seyfert 2 galaxy. From the X-ray variability pattern, we can estimate a likely lower limit of a few parsec to the distance of the inner walls of the torus in this object. Remarkably, IRAS 13218+0552 was not detected by XMM-Newton, despite being currently classified as a Seyfert 1 with a large [OIII] flux. However, the original classification was likely to be affected by an extreme velocity outflow component in the emission lines. The object likely harbors an highly obscured AGN and should be re-classified as a type 2 source.

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“…Stockton 1990;Hutchings & Neff 1992;Hutchings & Morris 1995;Boyce et al 1996;Bahcall et al 1997). The hosts of the NON and Wold sample objects frequently have projected close companions and a few display asymmetries or even tail-like features not expected of ellipticals.…”

Section: Comparisons To Host Colours Derived In Other Investigationsmentioning

confidence: 99%