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The violent youth of bright and massive cluster galaxies and their maturation over 7 billion years

Titulo: 
The violent youth of bright and massive cluster galaxies and their maturation over 7 billion years
Autores: 
Ascaso, B; Lemaux, BC; Lubin, LM; Gal, RR; Kocevski, DD; Rumbaugh, N; Squires, G
Resumen: 
In this study, we investigate the formation and evolution mechanisms of the brightest cluster galaxies (BCGs) over cosmic time. At high redshift (z similar to 0.9), we selected BCGs and most massive cluster galaxies (MMCGs) from the Cl1604 supercluster and compared them to low-redshift (z similar to 0.1) counterparts drawn from the MCXC meta-catalogue, supplemented by Sloan Digital Sky Survey imaging and spectroscopy. We observed striking differences in the morphological, colour, spectral, and stellar mass properties of the BCGs/MMCGs in the two samples. High-redshift BCGs/MMCGs were, in many cases, star-forming, late-type galaxies, with blue broad-band colours, properties largely absent amongst the low-redshift BCGs/MMCGs. The stellar mass of BCGs was found to increase by an average factor of 2.51 +/- 0.71 from z similar to 0.9 to z similar to 0.1. Through this and other comparisons, we conclude that a combination of major merging (mainly wet or mixed) and in situ star formation are the main mechanisms which build stellar mass in BCGs/MMCGs. The stellar mass growth of the BCGs/MMCGs also appears to grow in lockstep with both the stellar baryonic and total mass of the cluster. Additionally, BCGs/MMCGs were found to grow in size, on average, a factor of similar to 3, while their average Sersic index increased by similar to 0.45 from z similar to 0.9 to z similar to 0.1, also supporting a scenario involving major merging, though some adiabatic expansion is required. These observational results are compared to both models and simulations to further explore the implications on processes which shape and evolve BCGs/MMCGs over the past similar to 7 Gyr.
Autor principal: 
Ascaso, B
Autor/es del IAA: 
Ascaso, B.
DOI: 
10.1093/mnras/stu877
Revista: 
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Fecha de publicación: 
2014/07/21
Volumen: 
442
Issue: 
1
Páginas: 
589-615
Tipo de documento: 
Article
Palabras clave: 
techniques: photometric; techniques: spectroscopic; galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation

The ALHAMBRA Survey: Bayesian photometric redshifts with 23 bands for 3 deg(2)

Titulo: 
The ALHAMBRA Survey: Bayesian photometric redshifts with 23 bands for 3 deg(2)
Autores: 
Molino, A; Benitez, N; Moles, M; Fernandez-Soto, A; Cristobal-Hornillos, D; Ascaso, B; Jimenez-Teja, Y; Schoenell, W; Arnalte-Mur, P; Povic, M; Coe, D; Lopez-Sanjuan, C; Diaz-Garcia, LA; Varela, J; Stefanon, M; Cenarro, J; Matute, I; Masegosa, J; Marquez, I; Perea, J; Del Olmo, A; Husillos, C; Alfaro, E; Aparicio-Villegas, T; Cervino, M; Huertas-Company, M; Aguerri, JAL; Broadhurst, T; Cabrera-Cano, J; Cepa, J; Gonzalez, RM; Infante, L; Martinez, VJ; Prada, F; Quintana, JM
Resumen: 
The Advance Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) survey has observed eight different regions of the sky, including sections of the Cosmic Evolution Survey (COSMOS), DEEP2, European Large-Area Infrared Space Observatory Survey (ELAIS), Great Observatories Origins Deep Survey North (GOODS-N), Sloan Digital Sky Survey (SDSS) and Groth fields using a new photometric system with 20 optical, contiguous similar to 300-angstrom filters plus the JHKs bands. The filter system is designed to optimize the effective photometric redshift depth of the survey, while having enough wavelength resolution for the identification of faint emission lines. The observations, carried out with the Calar Alto 3.5-m telescope using the wide-field optical camera Large Area Imager for Calar Alto (LAICA) and the near-infrared (NIR) instrument Omega-2000, represent a total of similar to 700 h of on-target science images. Here we present multicolour point-spread function (PSF) corrected photometry and photometric redshifts for similar to 438 000 galaxies, detected in synthetic F814W images. The catalogues are complete down to a magnitude I similar to 24.5 AB and cover an effective area of 2.79 deg(2). Photometric zero-points were calibrated using stellar transformation equations and refined internally, using a new technique based on the highly robust photometric redshifts measured for emission-line galaxies. We calculate Bayesian photometric redshifts with the Bayesian Photometric Redshift (bpz)2.0 code, obtaining a precision of delta(z)/(1 + z(s)) = 1 per cent for I < 22.5 and delta(z)/(1 + z(s)) = 1.4 per cent for 22.5 < I < 24.5. The global n(z) distribution shows a mean redshift aEurozaEuro parts per thousand = 0.56 for I < 22.5 AB and aEurozaEuro parts per thousand = 0.86 for I < 24.5 AB. Given its depth and small cosmic variance, ALHAMBRA is a unique data set for galaxy evolution studies.
Autor principal: 
Molino, A
Autor/es del IAA: 
Molino, A.; Benitez, N.; Ascaso, B.; Jimenez-Teja, Y.; Schoenell, W.; Povic, M.; Matute, I.; Masegosa, J.; Marquez, I.; Perea, J.; Del Olmo, A.; Husillos, C.; Alfaro, E.; Aparicio-Villegas, T.; Cervino, M.; Gonzalez, R. M.; Prada, F.; Quintana, J. M.
DOI: 
10.1093/mnras/stu387
Revista: 
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Fecha de publicación: 
2014/07/11
Volumen: 
441
Issue: 
4
Páginas: 
2891-2922
Tipo de documento: 
Article
Palabras clave: 
methods: data analysis; techniques: photometric; catalogues; surveys; galaxies: distances and redshifts; galaxies: evolution; galaxies: photometry

COMPREHENSIVE MONITORING OF GAMMA-RAY BRIGHT BLAZARS. I. STATISTICAL STUDY OF OPTICAL, X-RAY, AND GAMMA-RAY SPECTRAL SLOPES

Titulo: 
COMPREHENSIVE MONITORING OF GAMMA-RAY BRIGHT BLAZARS. I. STATISTICAL STUDY OF OPTICAL, X-RAY, AND GAMMA-RAY SPECTRAL SLOPES
Autores: 
Williamson, KE; Jorstad, SG; Marscher, AP; Larionov, VM; Smith, PS; Agudo, I; Arkharov, AA; Blinov, DA; Casadio, C; Efimova, NV; Gomez, JL; Hagen-Thorn, VA; Joshi, M; Konstantinova, TS; Kopatskaya, EN; Larionova, EG; Larionova, LV; Malmrose, MP; McHardy, IM; Molina, SN; Morozova, DA; Schmidt, GD; Taylor, BW; Troitsky, IS
Resumen: 
We present gamma-ray, X-ray, ultraviolet, optical, and near-infrared light curves of 33 gamma-ray bright blazars over 4 years that we have been monitoring since 2008 August with multiple optical, ground-based telescopes and the Swift satellite, and augmented by data from the Fermi Gamma-ray Space Telescope and other publicly available data from Swift. The sample consists of 21 flat-spectrum radio quasars (FSRQs) and 12 BL Lac objects (BL Lacs). We identify quiescent and active states of the sources based on their gamma-ray behavior. We derive. gamma-ray, X-ray, and optical spectral indices, alpha(gamma), alpha(X), and alpha(o), respectively (F-nu alpha nu(alpha)), and construct spectral energy distributions during quiescent and active states. We analyze the relationships between different spectral indices, blazar classes, and activity states. We find (1) significantly steeper gamma-ray spectra of FSRQs than for BL Lacs during quiescent states, but a flattening of the spectra for FSRQs during active states while the BL Lacs show no significant change; (2) a small difference of alpha(X) within each class between states, with BL Lac X-ray spectra significantly steeper than in FSRQs; (3) a highly peaked distribution of X-ray spectral slopes of FSRQs at similar to-0.60, but a very broad distribution of alpha(X) of BL Lacs during active states; (4) flattening of the optical spectra of FSRQs during quiescent states, but no statistically significant change of alpha(o) of BL Lacs between states; and (5) a positive correlation between optical and gamma-ray spectral slopes of BL Lacs, with similar values of the slopes. We discuss the findings with respect to the relative prominence of different components of high-energy and optical emission as the flux state changes.
Autor principal: 
Williamson, KE
Autor/es del IAA: 
Agudo, Ivan; Casadio, Carolina; Gomez, Jose L.; Molina, Sol N.
DOI: 
10.1088/0004-637X/789/2/135
Revista: 
ASTROPHYSICAL JOURNAL
Fecha de publicación: 
2014/07/10
Volumen: 
789
Issue: 
2
Tipo de documento: 
Article
Palabras clave: 
BL Lacertae objects: general; galaxies: active; galaxies: jets; quasars: general
Número de artículo: 
135

The host of the SN-less GRB 060505 in high resolution

Titulo: 
The host of the SN-less GRB 060505 in high resolution
Autores: 
Thone, CC; Christensen, L; Prochaska, JX; Bloom, JS; Gorosabel, J; Fynbo, JPU; Jakobsson, P; Fruchter, AS
Resumen: 
The spiral host galaxy of the Swift GRB 060505 at z = 0.089 was the site of a puzzling long duration burst without an accompanying supernova. Studies of the burst environment by Thone et al. suggested that this Gamma-ray Burst (GRB) came from the collapse of a massive star and that the GRB site was a region with properties different from the rest of the galaxy. We reobserved the galaxy in high spatial resolution using the VIMOS integral-field unit at the VLT with a spaxel size of 0.67 arcsec. Furthermore, we use long-slit high-resolution data from HIRES/Keck at two different slit positions covering the GRB site, the centre of the galaxy and an H ii region next to the GRB region. We compare the properties of different H ii regions in the galaxy with the GRB site and study the global and local kinematic properties of this galaxy. The resolved data show that the GRB site has the lowest metallicity in the galaxy with similar to 1/3 Z(aS (TM)), but its specific star formation rate (SSFR) of 7.4 M-aS (TM) yr(-1)/L/L* and age (determined by the H alpha EW) are similar to other H ii regions in the host. The galaxy shows a gradient in metallicity and SSFR from the bulge to the outskirts as it is common for spiral galaxies. This gives further support to the theory that GRBs prefer regions of higher star formation and lower metallicity, which, in S-type galaxies, are more easily found in the spiral arms than in the centre. Kinematic measurements of the galaxy do not show evidence for large perturbations but a minor merger in the past cannot be excluded. This study confirms the collapsar origin of GRB 060505 but reveals that the properties of the H ii region surrounding the GRB were not unique to that galaxy. Spatially resolved observations are key to know the implications and interpretations of unresolved GRB hosts observations at higher redshifts.
Autor principal: 
Thone, CC
Autor/es del IAA: 
Thoene, C. C.; Gorosabel, J.
DOI: 
10.1093/mnras/stu711
Revista: 
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Fecha de publicación: 
2014/07/01
Volumen: 
441
Issue: 
3
Páginas: 
2034-2048
Tipo de documento: 
Article
Palabras clave: 
techniques: high angular resolution; gamma-ray bursts: individual: GRB 060505; galaxies: ISM; galaxies: kinematics and dynamics

Deriving model-based T-e-consistent chemical abundances in ionized gaseous nebulae

Titulo: 
Deriving model-based T-e-consistent chemical abundances in ionized gaseous nebulae
Autores: 
Perez-Montero, E
Resumen: 
The derivation of abundances in gaseous nebulae ionized by massive stars using optical collisionally excited emission lines is studied in this work, comparing the direct or T-e method with updated grids of photoionization models covering a wide range of input conditions of O/H and N/O abundances and ionization parameter. The abundances in a large sample of compiled objects with at least one auroral line are re-derived and later compared with the chi(2)-weighted-mean abundances from the models. The agreement between the abundances using the two methods both for O/H and N/O is excellent with no additional assumptions about the geometry or physics governing the H-II regions. Although very inaccurate model-based O/H are obtained when no auroral lines are considered, this can be overcome assuming empirical laws between O/H, log U, and N/O to constrain the considered models. In this way, for 12+log(O/H) > 8.0, a precision better than 0.1 dex consistent with the direct method is attained. For very low Z, models give higher O/H values and a high dispersion, possibly owing to the contamination of the low-excitation emission lines. However, in this regime, the auroral lines are usually well detected. The use of this procedure, in a publicly available script, HII-CHI-MISTRY, leads to the derivation of abundances in faint-/high-redshift objects consistent with the direct method based on collisionally excited lines.
Autor principal: 
Perez-Montero, E
Autor/es del IAA: 
Perez-Montero, E
DOI: 
10.1093/mnras/stu753
Revista: 
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Fecha de publicación: 
2014/07/01
Volumen: 
441
Issue: 
3
Páginas: 
2663-2675
Tipo de documento: 
Article
Palabras clave: 
methods: data analysis; ISM: abundances; galaxies: abundances

ANOTHER SHORT-BURST HOST GALAXY WITH AN OPTICALLY OBSCURED HIGH STAR FORMATION RATE: THE CASE OF GRB 071227

Titulo: 
ANOTHER SHORT-BURST HOST GALAXY WITH AN OPTICALLY OBSCURED HIGH STAR FORMATION RATE: THE CASE OF GRB 071227
Autores: 
Guelbenzu, AN; Klose, S; Michalowski, MJ; Savaglio, S; Kann, DA; Rossi, A; Hunt, LK; Gorosabel, J; Greiner, J; McKenzie, MRG; Palazzi, E; Schmidl, S
Resumen: 
We report on radio continuum observations of the host galaxy of the short gamma-ray burst 071227 (z = 0.381) with the Australia Telescope Compact Array. We detect the galaxy in the 5.5 GHz band with an integrated flux density of F-nu = 43 +/- 11 mu Jy, corresponding to an unobscured star-formation rate of about 24 M-circle dot yr(-1), 40 times higher than what was found from optical emission lines. Among the similar to 30 well-identified and studied host galaxies of short bursts this is the third case where the host is found to undergo an episode of intense star formation. This suggests that a fraction of all short-burst progenitors hosted in star-forming galaxies could be physically related to recent star formation activity, implying a relatively short merger timescale.
Autor principal: 
Guelbenzu, AN
Autor/es del IAA: 
Gorosabel, J.
DOI: 
10.1088/0004-637X/789/1/45
Revista: 
ASTROPHYSICAL JOURNAL
Fecha de publicación: 
2014/07/01
Volumen: 
789
Issue: 
1
Tipo de documento: 
Article
Palabras clave: 
gamma-ray burst: individual (GRB 071227)

THE HISTORY OF A QUIET-SUN MAGNETIC ELEMENT REVEALED BY IMaX/SUNRISE

Titulo: 
THE HISTORY OF A QUIET-SUN MAGNETIC ELEMENT REVEALED BY IMaX/SUNRISE
Autores: 
Requerey, IS; Iniesta, JCD; Rubio, LRB; Bonet, JA; Pillet, VM; Solanki, SK; Schmidt, W
Resumen: 
Isolated flux tubes are considered to be fundamental magnetic building blocks of the solar photosphere. Their formation is usually attributed to the concentration of magnetic field to kG strengths by the convective collapse mechanism. However, the small size of the magnetic elements in quiet-Sun areas has prevented this scenario from being studied in fully resolved structures. Here, we report on the formation and subsequent evolution of one such photospheric magnetic flux tube, observed in the quiet Sun with unprecedented spatial resolution (0 ''.15-0 ''.18) and high temporal cadence (33 s). The observations were acquired by the Imaging Magnetograph eXperiment on board the Sunrise balloon-borne solar observatory. The equipartition field strength magnetic element is the result of the merging of several same polarity magnetic flux patches, including a footpoint of a previously emerged loop. The magnetic structure is then further intensified to kG field strengths by convective collapse. The fine structure found within the flux concentration reveals that the scenario is more complex than can be described by a thin flux tube model with bright points and downflow plumes being established near the edges of the kG magnetic feature. We also observe a daisy-like alignment of surrounding granules and a long-lived inflow toward the magnetic feature. After a subsequent weakening process, the field is again intensified to kG strengths. The area of themagnetic feature is seen to change in anti-phase with the field strength, while the brightness of the bright points and the speed of the downflows varies in phase. We also find a relation between the brightness of the bright point and the presence of upflows within it.
Autor principal: 
Requerey, IS
Autor/es del IAA: 
Requerey, Iker S.; Del Toro Iniesta, Jose Carlos; Bellot Rubio, Luis R.
DOI: 
10.1088/0004-637X/789/1/6
Revista: 
ASTROPHYSICAL JOURNAL
Fecha de publicación: 
2014/07/01
Volumen: 
789
Issue: 
1
Tipo de documento: 
Article
Palabras clave: 
convection; magnetic fields; Sun: granulation; Sun: photosphere; techniques: polarimetric; techniques: spectroscopic
Número de artículo: 
6

ARE (PSEUDO)BULGES IN ISOLATED GALAXIES ACTUALLY PRIMORDIAL RELICS?

Titulo: 
ARE (PSEUDO)BULGES IN ISOLATED GALAXIES ACTUALLY PRIMORDIAL RELICS?
Autores: 
Lorenzo, MF; Sulentic, J; Verdes-Montenegro, L; Blasco-Herrera, J; Argudo-Fernandez, M; Garrido, J; Ramirez-Moreta, P; Ruiz, JE; Sanchez-Exposito, S; Santander-Vela, JD
Resumen: 
We present structural parameters and (g-i) bulge/disk colors for a large sample (189) of isolated AMIGA galaxies. The structural parameters of bulges were derived from the two-dimensional bulge/disk/bar decomposition of Sloan Digital Sky Survey i-band images using GALFIT. Galaxies were separated between classical bulges (n(b) > 2.5) and pseudobulges (n(b) < 2.5), resulting in a dominant pseudobulge population (94%) with only 12 classical bulges. In the <mu(e)>-R-e plane, pseudobulges are distributed below the elliptical relation (smaller R-e and fainter mu(e)), with the closest region to the Kormendy relation populated by those pseudobulges with larger values of B/T. We derived (g-i) bulge colors using aperture photometry and find that pseudobulges show median colors (g-i)(b) similar to 1.06, while their associated disks are much bluer, (g-i)(d) similar to 0.77. Moreover, 64% (113/177) of pseudobulges follow the red sequence of early-type galaxies. Bluer pseudobulges tend to be located in galaxies with the highest likelihood of tidal perturbation. The red bulge colors and low B/T values for AMIGA isolated galaxies are consistent with an early formation epoch and not much subsequent growth. Properties of bulges in isolated galaxies contrast with a picture where pseudobulges grow continuously via star formation. They also suggest that environment could be playing a role in rejuvenating the pseudobulges.
Autor principal: 
Lorenzo, MF
Autor/es del IAA: 
Fernandez Lorenzo, M.; Sulentic, J.; Verdes-Montenegro, L.; Blasco-Herrera, J.; Argudo-Fernandez, M.; Garrido, J.; Ramirez-Moreta, P.; Ruiz, J. E.; Sanchez-Exposito, S.; Santander-Vela, J. D.
DOI: 
10.1088/2041-8205/788/2/L39
Revista: 
ASTROPHYSICAL JOURNAL LETTERS
Fecha de publicación: 
2014/06/20
Volumen: 
788
Issue: 
2
Tipo de documento: 
Article
Palabras clave: 
galaxies: fundamental parameters; galaxies: general; galaxies: interactions
Número de artículo: 
L39

The SPARC Data Initiative: Comparison of upper troposphere/lower stratosphere ozone climatologies from limb-viewing instruments and the nadir-viewing Tropospheric Emission Spectrometer

Titulo: 
The SPARC Data Initiative: Comparison of upper troposphere/lower stratosphere ozone climatologies from limb-viewing instruments and the nadir-viewing Tropospheric Emission Spectrometer
Autores: 
Neu, JL; Hegglin, MI; Tegtmeier, S; Bourassa, A; Degenstein, D; Froidevaux, L; Fuller, R; Funke, B; Gille, J; Jones, A; Rozanov, A; Toohey, M; von Clarmann, T; Walker, KA; Worden, JR
Resumen: 
We present the first comprehensive intercomparison of currently available satellite ozone climatologies in the upper troposphere/lower stratosphere (UTLS) (300-70hPa) as part of the Stratosphere-troposphere Processes and their Role in Climate (SPARC) Data Initiative. The Tropospheric Emission Spectrometer (TES) instrument is the only nadir-viewing instrument in this initiative, as well as the only instrument with a focus on tropospheric composition. We apply the TES observational operator to ozone climatologies from the more highly vertically resolved limb-viewing instruments. This minimizes the impact of differences in vertical resolution among the instruments and allows identification of systematic differences in the large-scale structure and variability of UTLS ozone. We find that the climatologies from most of the limb-viewing instruments show positive differences (ranging from 5 to 75%) with respect to TES in the tropical UTLS, and comparison to a zonal mean ozonesonde climatology indicates that these differences likely represent a positive bias for p100hPa. In the extratropics, there is good agreement among the climatologies regarding the timing and magnitude of the ozone seasonal cycle (differences in the peak-to-peak amplitude of <15%) when the TES observational operator is applied, as well as very consistent midlatitude interannual variability. The discrepancies in ozone temporal variability are larger in the tropics, with differences between the data sets of up to 55% in the seasonal cycle amplitude. However, the differences among the climatologies are everywhere much smaller than the range produced by current chemistry-climate models, indicating that the multiple-instrument ensemble is useful for quantitatively evaluating these models.
Autor principal: 
Neu, JL
Autor/es del IAA: 
Funke, B.
DOI: 
10.1002/2013JD020822
Revista: 
JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
Fecha de publicación: 
2014/06/16
Volumen: 
119
Issue: 
11
Páginas: 
6971-6990
Tipo de documento: 
Article
Palabras clave: 
ozone climatologies; upper troposphere; lower stratosphere; satellite measurements

A simultaneous 3.5 and 1.3 mm polarimetric survey of active galactic nuclei in the northern sky

Titulo: 
A simultaneous 3.5 and 1.3 mm polarimetric survey of active galactic nuclei in the northern sky
Autores: 
Agudo, I; Thum, C; Gomez, JL; Wiesemeyer, H
Resumen: 
Context. Short millimeter observations of radio-loud active galactic nuclei (AGN) offer an excellent opportunity to study the physics of their synchrotron-emitting relativistic jets from where the bulk of radio and millimeter emission is radiated. On one hand, AGN jets and their emission cores are significantly less affected by Faraday rotation and depolarization than at longer wavelengths. On the other hand, the millimeter emission of AGN is dominated by the compact innermost regions in the jets, where the jet cannot be seen at longer wavelengths due to synchrotron opacity. Aims. We present the first simultaneous dual frequency 86 GHz and 229 GHz polarimetric survey of all four Stokes parameters for a large sample of 211 radio-loud active galactic nuclei, designed to be flux limited at 1 Jy at 86 GHz. Methods. Most of the observations were made in mid-August 2010 using the XPOL polarimeter on the IRAM 30 m millimetric radio telescope. Results. Linear polarization detections above a 3 sigma median level of similar to 1.0% are reported for 183 sources at 86 GHz and for 23 sources at 229 GHz, where the median 3s level is similar to 6.0%. We show a clear excess of the linear polarization degree that is detected at 229 GHz with regard to that at 86 GHz by a factor of similar to 1.6. This implies a progressively better ordered magnetic field for blazar jet regions that are located progressively upstream in the jet. We show that the linear polarization angle at 86 and 229 GHz and the jet structural position angle for both quasars and BL Lacs do not show a clear preference to align in either parallel or perpendicular directions. Our variability study with regard to the 86 GHz data from our previous survey points out a large degree of variation. In particular, we report total flux and linear polarization changes in time scales of years by median factors of similar to 1.5 in total flux and similar to 1.7 in linear polarization degree (with maximum variations by factors up to 6.3 and similar to 5, respectively). Moreover, 86% of sources show linear polarization angles evenly distributed with regard to our previous measurements.
Autor principal: 
Agudo, I
Autor/es del IAA: 
Agudo, I.; Gomez, J. L.
DOI: 
10.1051/0004-6361/201423366
Revista: 
ASTRONOMY & ASTROPHYSICS
Fecha de publicación: 
2014/06
Volumen: 
566
Tipo de documento: 
Article
Palabras clave: 
galaxies: active; galaxies: jets; quasars: general; BL Lacertae objects: general; polarization; surveys
Número de artículo: 
A59

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