On-axis spatially resolved spectroscopy of low redshift quasar host 
galaxies: HE 1503+0228, at $z=0.135$

Courbin, F.; Letawe, Géraldine; Magain, Pierre; Wisotzki, L.; Jablonka, P.; Jahnke, K.; Kuhlbrodt, B.; Alloin, D.; Meylan, G.; Minniti, D.; Burud, I.

doi:10.1051/0004-6361:20021246

Cited by 17 publications

(36 citation statements)

References 23 publications

(27 reference statements)

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“…The FORS2/MXU spectra of HE 0450-2958 are all deconvolved using the MCS algorithm for slit spectra (Magain et al 1998;Courbin et al 2000), allowing a separation of the QSO light from the underlying extended objects. This method has been used successfully on many occasions, either on data of QSO host galaxies (Courbin et al 2002;Letawe et al 2004;M05;Letawe et al 2007) or on data of gravitationally lensed QSOs (e.g., Eigenbrod et al 2006Eigenbrod et al , 2007.…”

Section: Slit Spectroscopymentioning

confidence: 99%

Slit and integral-field optical spectroscopy of the enigmatic quasar HE 0450–2958

Letawe¹,

Magain²,

Courbin

2008

A&A

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Context. Interest in the quasar HE 0450-2958 arose following the publication of the non-detection of its expected massive host, leading to various interpretations. Aims. This article investigates the gaseous and stellar contents of the system through additional VLT/FORS slit spectra and integral field spectroscopy from VLT/VIMOS. Methods. We apply our MCS deconvolution algorithm on slit spectra for the separation of the QSO and diffuse components, and develop a new method to remove the point sources in Integral Field Spectra, allowing extraction of velocity maps, narrow-line images, spatially resolved spectra or ionization diagrams of the surroundings of HE 0450-2958. Results. The whole system is embedded in gas, mostly ionized by the QSO radiation field and shocks associated with radio jets. The observed gas and star dynamics are unrelated, revealing a strongly perturbed system. Despite longer spectroscopic observations, the host galaxy remains undetected.

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Section: Slit Spectroscopymentioning

confidence: 99%

Slit and integral-field optical spectroscopy of the enigmatic quasar HE 0450–2958

Letawe¹,

Magain²,

Courbin

2008

A&A

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“…Because the lensing QSOs are at low redshift (z < 0.4), the range of follow-up applications is very rich, as their Hβ, Hα, [O iii] emission lines are clearly measurable in the SDSS spectra. In addition, the angular size and luminosity of their host galaxies make it possible to carry out direct spectroscopy of the host (e.g., Lewate et al 2007;A&A 516, L12 (2010) Letawe et al 2004;Courbin et al 2002). Our sample will therefore allow us to test directly the scaling laws established between the properties of QSO emission lines, the mass of the central black hole, and the total mass of the host galaxies (e.g., Kaspi et al 2005;Bonning et al 2005;Shen et al 2008).…”

Section: Introductionmentioning

confidence: 99%

First case of strong gravitational lensing by a QSO: SDSS J0013+1523 atz= 0.120

Courbin¹,

Tewes²,

Djorgovski

et al. 2010

A&A

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We present the first case of strong gravitational lensing by a QSO: SDSS J0013+1523 at z = 0.120. The discovery is the result of a systematic search for emission lines redshifted behind QSOs, among 22 298 spectra of the SDSS data release 7. Apart from the z = 0.120 spectral features of the foreground QSO, the spectrum of SDSS J0013+1523 also displays the [O ii] and Hβ emission lines and the [O iii] doublet, all at the same redshift, z = 0.640. Using sharp Keck adaptive optics K-band images obtained using laser guide stars, we unveil two objects within a radius of 2 from the QSO. Deep Keck optical spectroscopy clearly confirms one of these objects at z = 0.640 and shows traces of the [O iii] emission line of the second object, also at z = 0.640. Lens modeling suggests that they represent two images of the same z = 0.640 emission-line galaxy. Our Keck spectra also allow us to measure the redshift of an intervening galaxy at z = 0.394, located 3.2 away from the line of sight to the QSO. If the z = 0.120 QSO host galaxy is modeled as a singular isothermal sphere, its mass within the Einstein radius is M E (r < 1 h −1 kpc) = 2.16 × 10 10 h −1 M and its velocity dispersion is σ SIS = 169 km s −1 . This is about 1-σ away from the velocity dispersion estimated from the width of the QSO Hβ emission line, σ * (M BH ) = 124 ± 47 km s −1 . Deep optical HST imaging will be necessary to constrain the total radial mass profile of the QSO host galaxy using the detailed shape of the lensed source. This first case of a QSO acting as a strong lens on a more distant object opens new directions in the study of QSO host galaxies.

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“…The full sample, for which optical and near-IR imaging is also available (Jahnke 2002;Jahnke et al 2003Jahnke et al , 2004 will be fully described and analyzed in Letawe et al, in prep., while the deconvolution techniques used to decompose the data into two independent spectra of the unresolved central quasar and of the extended host galaxy are presented in Magain et al (1998) and Courbin et al (2000). A first application of these techniques to the quasar HE 1503+0228 is presented in Courbin et al (2002). It shows that the host of this quasar is a normal spiral galaxy with M(r < 10 kpc) = (1.9 ± 0.3) × 10 11 M and with stellar populations typical of a normal spiral galaxy.…”

Section: Introductionmentioning

confidence: 99%

On-axis spectroscopy of thez$\mathsf{=0.144}$ radio-loud quasar HE 1434–1600: an elliptical host with a highly ionized ISM

Letawe¹,

Courbin²,

Magain³

et al. 2004

A&A

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Abstract. VLT on-axis optical spectroscopy of the z = 0.144 radio-loud quasar HE 1434−1600 is presented. The spatially resolved spectra of the host galaxy are deconvolved and separated from those of the central quasar in order to study the dynamics of the stars and gas as well as the physical conditions of the ISM. We find that the host of HE 1434−1600 is an elliptical galaxy that resides in a group of at least 5 member galaxies, and that most likely experienced a recent collision with its nearest companion. Compared with other quasar host galaxies, HE 1434−1600 has a highly ionized ISM. The ionization state corresponds to that of typical Seyferts, but the ionized regions are not distributed in a homogeneous way around the QSO, and are located preferentially several kiloparsecs away from it. While the stellar absorption lines do not show any significant velocity field, the gas emission lines do. The observed gas velocity field is hard to reconcile with dynamical models involving rotating disk, modified Hubble laws or power laws, that all require extreme central masses (M > 10 9 M ) to provide only poor fit to the data. Power law models, which best fit the data, provide a total mass of M(<10 kpc) = 9.2 × 10 10 M . We conclude that the recent interaction between HE 1434−1600 and its closest companion has strongly affected the gas velocity and ionization state, from the center of the galaxy to its most external parts.

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On-axis spatially resolved spectroscopy of low redshift quasar host galaxies: HE 1503+0228, at $z=0.135$

Cited by 17 publications

References 23 publications

Slit and integral-field optical spectroscopy of the enigmatic quasar HE 0450–2958

Slit and integral-field optical spectroscopy of the enigmatic quasar HE 0450–2958

First case of strong gravitational lensing by a QSO: SDSS J0013+1523 atz= 0.120

On-axis spectroscopy of thez$\mathsf{=0.144}$ radio-loud quasar HE 1434–1600: an elliptical host with a highly ionized ISM

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