Issue |
A&A
Volume 511, February 2010
|
|
---|---|---|
Article Number | A27 | |
Number of page(s) | 4 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200913760 | |
Published online | 26 February 2010 |
A quasar companion to the puzzling quasar SDSS J0927+2943
(Research Note)
R. Decarli1,2 - R. Falomo3 - A. Treves1,4 - M. Barattini1
1 - Università degli Studi dell'Insubria, via Valleggio 11,
22100 Como, Italy
2 -
MPIA, Königstuhl 17, 69117, Heidelberg, Germany
3 -
INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5,
35122, Padova, Italy
4 -
Istituto Naz. Fis. Nucleare - Università di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy
Received 27 November 2009 / Accepted 23 December 2009
Abstract
We report the discovery of a quasar close to SDSS J0927+2943
(z = 0.713), which is a massive binary/recoiling black hole
candidate. The companion quasar is at a projected distance of
125
h70-1 kpc and exhibits a radial velocity difference of
1400 km s-1 with respect to the known quasar.
We discuss the nature of this peculiar quasar
pair and the properties of its environment. We propose that
the overall system is caught in the process of ongoing
structure formation.
Key words: quasars: general - quasars: emission lines - quasars: individual: SDSS J092712.65+294344.0
1 Introduction
Quasar pairs are usually divided in: i) physical pairs, in which the two quasars have similar redshift and belong to the same cosmological structure (e.g., Foreman et al. 2009); ii) gravitational lenses, where the light of a single quasar is split into two or more images due to the light bending of an intervening massive object (e.g. Wittman et al. 2000; Chieregato et al. 2007); iii) apparent pairs, resulting from chance projected associations. Each of the three classes has great importance for probing the galactic halos of quasar host galaxies (column density, metal and dust abundances, ionization, etc.), the distribution of matter from galactic to super-cluster scales, and the role of galaxy interactions in triggering nuclear activity. For instance, Kirkman & Tytler (2008) and Gallerani et al. (2008) used absorption features in the spectra of apparent quasar pairs to study the ionization properties of the gas in the halos of quasar hosts and to constrain the duty cycle of the nuclear activity. Zhdanov & Surdej (2001), Myers et al. (2007) and Hennawi et al. (2009,2006) used close, physical quasar pairs to show that the quasar correlation function gets progressively steeper at sub-megaparsec scales, where gravitational interactions among galaxies become stronger.
Quasar pairs are very rare: Only few tens of quasar pairs are known
with sub-arcmin separation (Hennawi et al. 2006; Veron-Cetty & Veron 2006). In a previous
work (Decarli et al. 2009a), we estimated that, given a quasar, the chance
probability of finding a companion quasar with
within
10'' is
(assuming the quasar number density by Croom et al. 2004). On the other hand, quasars belonging
to the same physical structure show significant clustering
(see, e.g., Coil et al. 2007; Shen et al. 2009; Bonoli et al. 2009). At very small angular
separations, the surface density of quasars within dense
environments is up to 3 orders of magnitude higher than in the field
(see, for instance, Hennawi et al. 2006; Wrobel & Laor 2009). Wide-field
surveys, such as the Sloan Digital Sky Survey (SDSS; see York et al. 2000) collected spectra of
100 000 quasars, but missed
most of close pairs because of the finite physical dimension of the
spectroscopic fibers. On the other hand, the enormous, multi-band
imaging database of the SDSS allows the search for quasar candidates
starting from their photometry. For instance, Hennawi et al. (2009)
employed colour-selection techniques and spectroscopic follow-up
observations to discover 24 new physical quasar pairs at
3.0 < z <
4.5.
In this framework, we started a programme to search for low-redshift
quasar pairs with small separations, starting from the SDSS photometric
dataset (Decarli et al., in preparation; see also Decarli et al. 2009a,b).
Low-redshift quasars have optical Spectral Energy Distributions (SEDs)
similar to those of blue stars (see, e.g., Richards et al. 2002).
Starting from the z<1 quasars in the spectroscopic catalogue by
Schneider et al. (2007), we searched for quasar companions in the SDSS
photometric database with projected separation below 200
h70-1 kpc (at the redshift of the known quasar). Quasar companion candidates
are selected on the basis of their colours, independently of the properties
of the reference quasars. We limited our study to Galactic
latitude
to minimize contaminations from stars.
About one hundred quasar pairs are selected in this way. For twenty
of them the companion object was also detected by the GALaxy
Evolution EXplorer (GALEX; Siegmund et al. 2004) in the FUV and
NUV bands. For these systems, we designed a plan of follow-up
spectroscopic observations at the Asiago Telescope, in order to
confirm the quasar classification and to study the properties of the
quasar pair.
Within this line of research, which at the moment had covered only few objects,
here we present the discovery of a companion quasar of the peculiar
quasar SDSS J092712.65+294344.0 (hereafter, S0927), a promising massive black
hole binary / recoiling black hole candidate (see Sect. 2).
The present discovery of a second quasar with
km s-1along the line of sight and projected separation
125
h70-1kpc adds new, unexpected elements for our comprehension of S0927.
In Sect. 3 we present our observations and the
data reduction. Results are given in Sect. 4.
In Sect. 5 we discuss the nature of this quasar pair,
focussing in particular on its environment.
Throughout the paper, we adopt a concordance cosmology
with H0=70 km s-1 Mpc-1,
,
.
2 The unusual quasar SDSS J0927+2943
S0927 (RA(J2000):
,
Dec(J2000):
;
u=18.69, g=18.42,
r=18.40, i=18.40, z=18.34) is a puzzling quasar,
discovered by Komossa et al. (2008) out of the enormous SDSS
spectroscopic database. It shows two sets of narrow emission lines
at different redshifts (hereafter, the ``blue'' system at
and the ``rest-frame'' system at
;
km s-1), and a set of broad emission lines at
.
The existence of another set of emission lines at
was claimed by Shields et al. (2009), mainly based on
the detection of an emission line at 8526 Å, identified with the
[O III]
.
We note however that this line is also
consistent with the Fe II
at
,
a
common feature in quasar spectra.
Three scenarios have been proposed to explain the velocity
difference between
and
:
Komossa et al. (2008) suggested that the active black hole (BH)
in this object is recoiling as the result of the coalescence of
two massive BHs; Dotti et al. (2009) and Bogdanovic et al. (2009)
proposed that the active black hole is part of a massive BH
binary with sub-parsec separation; finally Heckman et al. (2009) proposed
that the velocity difference in the two systems in S0927 is due
to the ongoing merger event between a massive galaxy, hosting the quasar,
and a satellite (responsible of the emission of narrow lines at
). This last scenario relies on the assumption
of a close alignment between the two galaxies, which is statistically
acceptable only if S0927 resides in a rich cluster. Furthermore, the
potential well of a rich galaxy cluster would explain the velocity
difference between the two emission line systems in S0927. On the
other hand, Decarli et al. (2009c) showed that the field of this object is not as
rich as the cluster scenario requires, the number of possible galaxy
candidates being consistent with a rich group in the best case.
3 Observations and data reduction
The optical spectrum of S0927 was collected with the 1.82 m Cima
Ekar telescope at the Asiago Observatory on January, 4, 2009. The
Asiago Faint Object Spectrograph Camera was mounted in long-slit
spectroscopy configuration with grism #4, yielding a spectral
resolutions of
(2.10'' slit) in the spectral range
3500-7800 Å (
Å). At
Å the spectral instrumental resolution is
17 Å. The slit was oriented with Position
,
so that the spectrum of the blue source placed
17.5'' south-west of the main target could be simultaneously
acquired (see Fig. 1). The total integration time was
100 min.
The standard IRAF
procedure was adopted in the data reduction. The
ccdred
package was employed to perform bias subtraction, flat field
correction, frame alignment and image combination. Cosmic rays were
eliminated with the cosmicrays
task in the crutils
package. The spectra extraction, the background subtraction and the
calibrations both in wavelength and in flux were performed with
doslit
task in specred
package, using a Hg-Cd lamps
and the spectrophotometric standard star Feige 34 as reference.
Wavelength calibration residuals are around 0.2 Å (sub-pixel).
Absolute calibration of spectra was optimized through the photometry
of field stars, by comparing corollary imaging with Johnson's Rfilters to the magnitudes published in the US Naval Observatory
catalogue. The uncertainty in the flux calibration is 0.1 mag.
Galactic extinction was accounted for according to the Galactic
H I maps by Schlegel, Finkbeiner & Davis (1998) and assuming RV = 3.1.
The spectra of the two sources are shown in Fig. 2.
![]() |
Figure 1: The field of S0927 as imaged in the r band from the SDSS. The slit orientation adopted in our new observation is also plotted. |
Open with DEXTER |
![]() |
Figure 2:
Our new spectra of S0927 and its (fainter) companion.
Main emission lines in the spectrum of S0927 are labelled
(see also Komossa et al. 2008). The Earth symbols mark relevant
atmospheric absorption features. Note the detection of the Mg II
line in the spectrum of quasar B and a tentative detection of
H |
Open with DEXTER |
Table 1: Properties of the detected emission lines.
4 Results
![]() |
Figure 3:
The Spectra Energy Distributions of S0927 and its companion.
Observed spectra are plotted as solid lines, while photometry data
are reported as circles. The quasar composite spectrum derived in
Decarli et al. (2010) is also shown for comparison (dotted line). FUV
and NUV fluxes derived from the GALEX archives. The magnitudes
in the optical bands are from the SDSS. The |
Open with DEXTER |
The blue object selected as a quasar candidate 17.5'' far from
S0927 (SDSS J092713.82+294335.5; RA(J2000):
,
Dec(J2000):
;
u=19.38, g=19.18, r=19.14, i=19.01, z=19.13)
appears in the USNO-A2 catalogue (Monet et al. 1998). The GALEX All-Sky
Survey provides estimates of its UV magnitudes (FUV =
,
NUV =
). The blue optical colours
and the bright UV emission are consistent with the typical Spectral
Energy Distribution (SED) of a quasar (see Fig.
3 and Decarli et al. 2009c). The spectrum shows a broad emission
line at 4772 Å and another possible emission line at 7395Å (see Fig. 2 and Table 1). We
identify the former with the Mg II and the latter with H
,
yielding z=0.705. Other identifications of the 4772 Å line
(e.g., with C IV) are ruled out by the lack of any correspondence
with other expected bright UV lines, e.g., C III], Si IV
and Ly
.
No obvious detection of the [O II] doublet
is reported. We fitted the profiles of these lines and
of the main lines in the spectrum of S0927 with gaussian profiles
(a superposition of 2 Gaussian is used for the Mg II line; see
the discussion on the fit of quasar broad emission lines in Decarli et al. 2010).
Table 1 reports the best fit parameters for the peak
wavelength and corresponding z, for the line width (as measured in the
observed frame) and for the line equivalent width. Referring to standard
techniques for single-epoch spectra of quasar (e.g., Decarli et al. 2010), we
infer the BH mass of the newly discovered quasar from the continuum
luminosity and the Mg II line width:
.
The uncertainty on
is of a factor
2, dominated
by the dispersion on the adopted broad line region radius-luminosity
relation.
The corresponding Eddington ratio is
= 0.22, assuming the
bolometric correction L/
(Richards et al. 2002).
5 Discussion and conclusions
The observations of the quasar pair presented here reveal a puzzling
nature. The probability that the pair is due to a chance superposition
is very small: Following Decarli et al. (2009a), we estimate that the probability
to find a companion quasar
with mb<20 and angular separation <20'' at any
redshift is 10-3. If we consider pairs
with redshift difference <1500 km s-1, the probability drops by
two orders of magnitude. Hence, at most one quasar pair with
properties similar to those observed in the case of S0927 is expected
among the
77 000 quasars in the SDSS catalogue by Schneider et al. (2007).
Therefore the chance superposition is very unlikely.
Alternatively, the two quasars may belong to a common physical structure,
as suggested by their velocity difference (-1400 km s-1 with
respect to
,
km s-1 with respect to
).
Quasars show some evidence of clustering in a way
that roughly resembles what observed in quiescent galaxies
(Coil et al. 2007; Shen et al. 2009; Söchting et al. 2002). Different environments are
observed depending on the radio loudness (Barr et al. 2003; Söchting et al. 2004) or on
other AGN properties (e.g., Hickox et al. 2009). Boris et al. (2007) analyzed
the environment of 4 quasar pairs at
,
and found evidence of
rich galaxy environment in 3 of them, while one pair (QP 0114-3140)
appears isolated. Djorgovski et al. (2007) discovered a quasar triplet
at z=2.076, with relative velocities of few hundrends km/s. The presence
of many galaxies in the field around the triplet suggests that
its environment may be particularly dense.
In the case of the quasar pair of S0927, if we assume that the two
objects are gravitationally bound, their velocity difference and projected
separation imply a dynamical mass of 1014
(depending on the
de-projected separation and the direction of the velocity vector).
Decarli et al. (2009c) reported that the number of galaxies around this system is
consistent with the presence of at most a moderately rich galaxy group.
Unless extreme Mass-to-Light ratios are invoked, this would suggest
that the system is not virialized. This quasar pair might thus unveil the
occurrence of an ongoing structure formation, similarly to the
low-redshift cases of the Blue Infalling Group (Cortese et al. 2006; Gavazzi et al. 2003),
the Stephan's Quintet (Sulentic et al. 2001) or the Cartwheel's system
(Wolter et al. 1999; Taylor & Atherton 1984).
The main difference among these low-z counter-parts and S0927 is
that none of the former examples shows quasar-like nuclear activity
in any galaxies (but note that NGC 7319 in the Stephan's Quintet
is a Seyfert 2). We remark here that a systematic, spectroscopic study
of the galaxies observed in the field of S0927 is mandatory to definitely
pin down the dynamical state of this system. Further, deep images
both in the optical and X-ray bands would also provide new contraints on
the mass and structure of the galactic environment of this pair.
Our results provide additional clues supporting the presence of a galaxy group surrounding S0927. This kind of structure is the ideal habitat for strong gravitational interactions to occur, which may trigger quasar-like nuclear activity (Canalizo et al. 2007; Bennert et al. 2008,2010). Alltogether, the available information about this system support a view in which a recent or ongoing galaxy merger is present. On the other hand, the projected distance and the relative velocity of the quasar pair are too high to account per se for explaining the occurrence of two emission line systems in S0927, which appears independent of the presence of a companion quasar. Deep, high-resolution multi-band images and multi-object spectroscopy of the sources in this field are required to probe the actual build-up of a galaxy group, to search for signatures of gravitational interactions, and to pin down the dynamics of the system.
AcknowledgementsWe thank the referee for his/her useful comments. R.D. thanks Massimo Dotti for useful discussions on the nature of this system. This work was based on observations collected at Asiago observatory. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
References
- Barr, J. M., Bremer, M. N., Baker, J. C., & Lehnert, M. D. 2003, MNRAS, 346, 229 [NASA ADS] [CrossRef] [Google Scholar]
- Bennert, N., Canalizo, G., Jungwiert, B., et al. 2008, ApJ, 677, 846 [NASA ADS] [CrossRef] [Google Scholar]
- Bennert, N., Treu, T., Woo, J. H., et al. 2010, ApJ, 708, 1507 [NASA ADS] [CrossRef] [Google Scholar]
- Bogdanovic, T., Eracleous, M., & Sigurdsson, S. 2009, ApJ, 697, 288 [NASA ADS] [CrossRef] [Google Scholar]
- Bonoli, S., Marulli, F., Springel, V., et al. 2009, MNRAS, 396, 423 [NASA ADS] [CrossRef] [Google Scholar]
- Boris, N. V., Sodré, L. Jr., Cypriano, E. S., et al. 2007, ApJ, 666, 747 [NASA ADS] [CrossRef] [Google Scholar]
- Canalizo, G., Bennert, N., Jungwiert, B., et al. 2007, ApJ, 669, 801 [NASA ADS] [CrossRef] [Google Scholar]
- Chieregato, M., Miranda, M., & Jetzer, P. 2007, A&A, 474, 777 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Coil, A. L., Hennawi, J. F., Newman, J. A., Cooper, M. C., & Davis, M. 2007, ApJ, 654, 115 [NASA ADS] [CrossRef] [Google Scholar]
- Cortese, L., Gavazzi, G., Boselli, A., et al. 2006, A&A, 453, 847 [Google Scholar]
- Croom, S. M., Schade, D., Boyle, B. J., et al. 2004, ApJ, 606, 126 [NASA ADS] [CrossRef] [Google Scholar]
- Decarli, R., Treves, A., & Falomo, R. 2009a, MNRAS Lett., 396, 31 [NASA ADS] [Google Scholar]
- Decarli, R., Dotti, M., Falomo, R., et al. 2009b, ApJ, 703, L76 [NASA ADS] [CrossRef] [Google Scholar]
- Decarli, R., Reynolds, M. T., & Dotti, M. 2009c, MNRAS, 397, 458 [NASA ADS] [CrossRef] [Google Scholar]
- Decarli, R., Falomo, R., Treves, A., et al. 2010, MNRAS, accepted, [arXiv:0911.2983] [Google Scholar]
- Djorgovski, S. G., Courbin, F., Meylan, G., et al. 2007, ApJ, 662, L1 [NASA ADS] [CrossRef] [Google Scholar]
- Dotti, M., Montuori, C., Decarli, R., et al. 2009, MNRAS Lett., 398, 73 [Google Scholar]
- Foreman, G., Volonteri, M., & Dotti, M. 2009, ApJ, 693, 1554 [NASA ADS] [CrossRef] [Google Scholar]
- Gallerani, S., Ferrara, A., Fan, X., & Choudhury, T. R. 2008, MNRAS, 386, 359 [NASA ADS] [CrossRef] [Google Scholar]
- Gavazzi, G., Cortese, L., Boselli, A., et al. 2003, ApJ, 597, 210 [NASA ADS] [CrossRef] [Google Scholar]
- Heckman, T. M., Krolik, J. H., Moran, S. M., Schnittman, J., & Gezari, S. 2009, ApJ, 695, 363 [NASA ADS] [CrossRef] [Google Scholar]
- Hennawi, J. F., Strauss, M. A., Oguri, M., et al. 2006, AJ, 131, 1 [NASA ADS] [CrossRef] [Google Scholar]
- Hennawi, J. F., Myers, A. D., Shen, Y., et al. 2009, ApJ, submitted [arXiv:0908.3907] [Google Scholar]
- Hickox, R. C., Jones, C., Forman, W. R., et al. 2009, ApJ, 696, 891 [Google Scholar]
- Kirkman, D., & Tytler, D. 2008, MNRAS, 391, 1457 [NASA ADS] [CrossRef] [Google Scholar]
- Komossa, S., Zhou, H., & Lu, H. 2008, ApJ, 678, L81 [NASA ADS] [CrossRef] [Google Scholar]
- Monet, D. 1998, USNO2 Catalogue, 1 [Google Scholar]
- Myers, A. D., Brunner, R. J., Richards, G. T., et al. 2007, ApJ, 658, 99 [NASA ADS] [CrossRef] [Google Scholar]
- Richards, G. T., Fan, X., Newberg, H. J., et al. 2002, AJ, 123, 2945 [NASA ADS] [CrossRef] [Google Scholar]
- Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525 [NASA ADS] [CrossRef] [Google Scholar]
- Schneider, D. P., Hall, P. B., Richards, G. T., et al. 2007, AJ, 134, 102 [NASA ADS] [CrossRef] [Google Scholar]
- Shen, Y., Greene, J. E., Strauss, M. A., Richards, G. T., & Schneider, D. P. 2008, ApJ, 680, 169 [NASA ADS] [CrossRef] [Google Scholar]
- Shen, Y., Strauss, M. A., Ross, N. P., et al. 2009, ApJ, 697, 1656 [NASA ADS] [CrossRef] [Google Scholar]
- Shields, G. A., Bonning, E. W., & Salviander, S. 2009, ApJ, 696, 1367 [NASA ADS] [CrossRef] [Google Scholar]
- Siegmund, O. H. W., Welsh, B. Y., Martin, C., et al. 2004, SPIE, 5488, 13 [NASA ADS] [CrossRef] [Google Scholar]
- Söchting, I. K., Clowes, R. G., & Campusano, L. E. 2002, MNRAS, 331, 569 [NASA ADS] [CrossRef] [Google Scholar]
- Söchting, I. K., Clowes, R. G., & Campusano, L. E. 2004, MNRAS, 347, 1241 [NASA ADS] [CrossRef] [Google Scholar]
- Sulentic, J. W., Rosado, M., Dultzin-Hacyan, D., et al. 2001, AJ, 122, 2993 [NASA ADS] [CrossRef] [Google Scholar]
- Taylor, K., & Atherton, P. D. 1984, MNRAS, 208, 601 [NASA ADS] [Google Scholar]
- Veron-Cetty, M. P., & Veron, P. 2006, A&A, 455, 773 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Vivek, M., Srianand, R., Noterdaeme, P., Mohan, V., & Kuriakose, V. C. 2009, MNRAS, 400, L6 [NASA ADS] [Google Scholar]
- Wittman, D. M., Tyson, J. A., Kirkman, D., Dell'Antonio, I., & Bernstein, G. 2000, Nature, 405, 143 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
- Wolter, A., Trinchieri, G., & Iovino, A. 1999, A&A, 342, 41 [NASA ADS] [Google Scholar]
- Wrobel, J. M., & Laor, A. 2009, ApJ, 699, L22 [NASA ADS] [CrossRef] [Google Scholar]
- York, D. G., Adelman, J., Anderson, J. E. Jr., et al. 2000, AJ, 120, 1579 [Google Scholar]
- Zhdanov, V. I., & Surdej, J. 2001, A&A, 372, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Footnotes
- ... J0927+2943
- Based on observations collected at Asiago observatory.
- ... IRAF
- IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.
All Tables
Table 1: Properties of the detected emission lines.
All Figures
![]() |
Figure 1: The field of S0927 as imaged in the r band from the SDSS. The slit orientation adopted in our new observation is also plotted. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Our new spectra of S0927 and its (fainter) companion.
Main emission lines in the spectrum of S0927 are labelled
(see also Komossa et al. 2008). The Earth symbols mark relevant
atmospheric absorption features. Note the detection of the Mg II
line in the spectrum of quasar B and a tentative detection of
H |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
The Spectra Energy Distributions of S0927 and its companion.
Observed spectra are plotted as solid lines, while photometry data
are reported as circles. The quasar composite spectrum derived in
Decarli et al. (2010) is also shown for comparison (dotted line). FUV
and NUV fluxes derived from the GALEX archives. The magnitudes
in the optical bands are from the SDSS. The |
Open with DEXTER | |
In the text |
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