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Emission Lines Properties of the Radio-Loud Quasar LAMOST J1131+3114 (Research Note)

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Emission Lines Properties of the Radio-Loud Quasar LAMOST J1131+3114 (Research Note) A&A 564, A89 (2014) Astronomy DOI: 10.1051/0004-6361/201321750 & c ESO 2014 Astrophysics Emission lines properties of the radio-loud quasar LAMOST J1131+3114 (Research Note) Z. X. Shi1,2,3,G.Comte2,4,A.L.Luo2,Y.H.Zhao2,J.K.Zhao2,5,T.D.Oswalt5,andF.C.Wu1 1 National Laboratory of Pattern Recognition, Institute of Automation, Chinese Academy of Sciences, 100190 Beijing, PR China 2 Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing, PR China e-mail: [email protected], [email protected] 3 University of Chinese Academy of Sciences, 100049 Beijing, PR China 4 Aix-Marseille Université, CNRS, Institut Pythéas, L.A.M., UMR 7326, 13388 Marseille Cedex, France 5 Physics and Space Science Department, Florida Institute of Technology, Melbourne FL 32901, USA Received 20 April 2013 / Accepted 24 February 2014 ABSTRACT The radio-loud quasar LAMOST J1131+3114 (Ton 580, B2 1128+315), showing asymmetrical profile in Hβ and [O III] lines, has been selected from the LAMOST Pilot Survey for further study. We present an analysis of its emission lines by means of multiple Gaussian fitting, performed on LAMOST, Apache Point Observatory, and archival spectra. The broad line region, with an Hβ line of FWHM ∼ 4000 km s−1 has been fit with a double Gaussian, one of which is very broad and redshifted from the reference frame. The object is a likely Population B quasar. The [O III] λλ4959, 5007 lines profiles of the source have been formally fit with two Gaussian components, one of which is as broad as ∼700 km s−1. This broader component, if physically meaningful, appears to be subject to moderate velocity shock excitation. The forbidden line ratios correspond to a poorly populated area in standard diagnostic diagrams of AGN narrow line regions. Key words. quasars: individual: LAMOST J1131+3114 – quasars: emission lines – galaxies: jets – galaxies: interactions – galaxies: kinematics and dynamics 1. Introduction 2. Literature, new spectra and archival data The geometry and kinematics of the broad line region (BLR) 2.1. Summary of previous work in active galactic nuclei (AGNs) have been studied for a long time, but still remain unexplained. Zamfir et al. (2010)ex- The radio-loud quasar LAMOST J1131+3114, an UV excess plore the properties of the Hβ emission line profile in a large, source in the Tonantzintla survey (Ton 580: Iriarte & Chavira homogeneous, and bright sample of N ∼ 470 low redshift 1957), was first detected at 408 MHz in Colla et al. (1970)and quasars extracted from Sloan Digital Sky Survey (DR5). Their listed in the Second Bologna Catalog (B2). Its redshift is z = results give further support to the concept of two populations A 0.289 (Hewitt & Burbidge 1980). Classified as a single compo- and B (with line FWHM, respectively, narrower and broader than nent radio source with a flat spectrum by Fanti et al. (1975), it has 4000 km s−1; Sulentic et al. 2007). Hu et al. (2008) report on a been mapped at 1.4 GHz in the FIRST survey, where it exhibits a systematic investigation of the Hβ and Fe II emission lines in a curved extended jet/lobe protruding out of the dominating com- sample of 568 quasars within z < 0.8 selected from the SDSS pact radio core towards the east. Kimball et al. (2011) classify and suggest the existence of an intermediate FWHM region. it as a J (core + jet) quasar and Snellen et al. (2002)asaflat Some sources have asymmetric and shifted Hβ profiles, sug- spectrum radio quasar (FSRQ). Assuming isotropic emission, gesting that the BLR has a structure more complex than a sin- the radio luminosity at 1.4 GHz is log L1400 = 32.9 for an optical = . −1 −1 gle virialized component (Marziani et al. 1996, 2003). We have (V band) luminosity of log L5500 Å 30 6(L in erg s Hz ). visually inspected all quasar spectra, which produced by the Unlike most FSRQ, optical variability and optical polarization Pilot Sky Survey of LAMOST. An object exhibiting asymmet- remain undetected (see, e.g., Stalin et al. 2004a,b; Stockman ric [O III] line profiles and an extended red wing of Hβ has et al. 1984) and the 1.4 GHz polarized flux fraction is very low. been selected for further study: LAMOST J113109.5+311405.4 From a 5 GHz VLBA map (Helmboldt et al. 2007), FIRST, and (hereafter LAMOST J1131+3114), a radio-loud quasar already NVSS maps, a Fanaroff-Riley type II seems unlikely. The ra- known as Ton 580 or B2 1128+315. dio loudness (Kellermann et al. 1989)isR ∼ 80 for the core We report on the analysis of several spectra of this source, alone and R ≥ 105 for the whole source (Helmboldt et al. 2007). including archival data. In Sect. 2, we briefly review the liter- The spectral index is −0.63 between 74 MHz and 8.4 GHz. This ature on this object, present our LAMOST and Apache Point quasar should be a young, core dominated source using the clas- Observatory (hereafter APO) spectra and summarize the archival sification of Zamfir et al. (2008). data. In Sect. 3, we present the multicomponent spectral line fit- Stockton (1978) measured redshifts of two faint galaxies ting and its results. In Sect. 4, we discuss the characterization of at 7 SE and 35 SW from the quasar (30 kpc and 150 kpc in BLR and narrow line region (NLR). projected distance) and found values very close to the quasar Article published by EDP Sciences A89, page 1 of 4 A&A 564, A89 (2014) redshift, showing evidence for its belonging to a physical group 100 of objects. 80 PM1996 The optical spectrum of LAMOST J1131+3114 has been 60 studied by several authors. Eracleous & Halpern (1994) from 40 a 6 Å resolution spectrum covering Hα found a broad line with 20 a full width at zero intensity of 22 000 km s−1 and a FWHM 0 of 4000 km s−1. Corbin (1997) shows a spectrum where what −5 he calls the “blue bump” (yielding the UV excess in imagery) 0 ) −5 is obvious, with very weak Fe II broad lines. Marziani et al. 1 − ˚ A (2003) studied the Hβ line range and confirmed a low value of 2 80 LAM2011 − Fe II blends for our object. They found an asymmetric Hβ line cm 60 1 profile with a weak, redshifted barycenter, very broad compo- − 40 nent extending beyond 5000 Å in rest frame. Grupe et al. (2004) erg s 20 17 also gave low values of Fe II equivalent width and Fe II/Hβ ratios. − 0 (10 λ Finally, the X-ray properties of this source were studied us- F −5 ing the Einstein Observatory (Shastri et al. 1993; and Wilkes 0 et al. 1994), ROSAT (Brinkmann et al. 1995), XMM-Newton −5 (Page et al. 2004), and Swift (Grupe et al. 2010). Page et al. 80 APO2012 (2004) showed evidence of a soft X-ray excess in the spectrum. 60 Giommi et al. (2012) did not detect LAMOST J1131+3114 in γ 40 -ray or submillimeter ranges using Fermi and Planck. 20 0 2.2. New observations −5 0 The LAMOST instrument is a multi-object spectroscopic facil- −5 ity able to take 4000 spectra of objects distributed across a field 4700 4750 4800 4850 4900 4950 5000 5050 5100 5150 Rest Wavelength (A˚) of 25 square degrees simultaneously in a single exposure (Cui et al. 2012). The spectral range extends from 3700 repeat unit Fig. 1. Hβ and [O III] emission line fitting of LAMOST J1131+3114. to 9000 Å with a resolution of R = 1800. Prefiguring the large PM1996: Marziani et al. (2003) (1996 May 22), LAM2011: LAMOST LAMOST survey of 10 million objects, a Pilot Survey was ini- (2011 December 24), APO2012: Apache Point Obs. (2012 June 15). Black: original spectra, red: the Gaussian components, blue: sum of tiated on 2011 Oct. 24 for extensive performance evaluation. components. The bottom panels show the residuals. LAMOST J1131+3114, was observed on 2011 December 24, targeted by fiber 51 of spectrograph number 15. The raw data have been reduced using the LAMOST data reduction pipeline Hγ and [O III] λ4363. After proper normalization on the peak and only a coarse relative flux calibration was applied (Luo et al. flux density of [O III] λ5007, the five spectra are very consistent, 2004, 2012). implying overall temporal stability in the emission lines fluxes Follow-up observations of LAMOST J1131+3114 were across 15 years. made with the Double Imaging Spectrograph on the ARC 3.5 m telescope at APO on 2012 June 15. The spectrograph was used in high-resolution mode (2 Å/pixel) with a 1.5 slit (6 kpc) 3. Data analysis oriented east-west. The gratings were centered at 6800 Å 3.1. Multicomponent fitting of Hβ and [O III] lines (red) and 4400 Å (blue), yielding wavelength coverages of β + 6200−7600 Å and 3800−5000 Å, unfortunately slightly too red The H line of LAMOST J1131 3114 shows a sharp peak su- to cover completely the Hβ line profile of the source shotward of perimposed over a much broader and asymmetric profile, with a very broad and weak wing extending even beyond [O III] λ5007. 4815 Å (in rest frame). Owing to the Fe II emission weakness, we have assumed that The data were reduced with IRAF reduction procedures, the principal contributor to the local background below the following the usual path (bias, flats, HeNe arc, flux standard) [O III] lines is the Hβ red broad tail.
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