The Fourth Data Release of the Sloan Digital Sky Survey

Adelman-McCarthy, Jennifer K.; Agüeros, Marcel A.; Allam, S.; Anderson, K. S. J.; Anderson, Scott F.; Annis, J.; Bahcall, Neta A.; Baldry, I. K.; Barentine, John C.; Berlind, Andreas A.; Bernardi, Mariangela; Blanton, Michael R.; Boroski, William N.; Brewington, H.; Brinchmann, Jarle; Brinkmann, J.; Brunner, Róbert; Budavàri, Tamás; Carey, Larry N.; Carr, Michael; Castander, F. J.; Connolly, Andrew J.; Csabai, István; Czarapata, Paul C.; Dalcanton, Julianne J.; Doi, Mamoru; Dong, Feng; Eisenstein, Daniel J.; Evans, Michael L.; Fan, Xiaohui; Finkbeiner, Douglas P.; Friedman, S. D.; Frieman, Joshua A.; Fukugita, M.; Gillespie, Bruce; Glazebrook, Karl; Gray, Jim; Grebel, Eva K.; Gunn, James E.; Gurbani, Vijay K.; Haas, E. de; Hall, Patrick B.; Harris, Frederick H.; Harvanek, Michael; Hawley, Suzanne L.; Hayes, J. J. E.; Hendry, John S.; Hennessy, G. S.; Hindsley, Robert B.; Hirata, Christopher M.; Hogan, Craig J.; Hogg, David W.; Holmgren, D.; Holtzman, Jon A.; Ichikawa, S.; Ivezić, Željko; Jester, Sebastian; Johnston, David; Jorgensen, A. M.; Jurić, Mario; Kent, Stephen M.; Kleinman, S. J.; Knapp, G. R.; Kniazev, A. Y.; Krön, Richard G.; Krzesiński, Jurek; Kuropatkin, N.; Lamb, D. Q.; Lampeitl, H.; Lee, Brian C.; Leger, R. French; Lin, Huan; Long, Daniel C.; Loveday, Jon; Lupton, Robert H.; Margon, B.; Martínez–Delgado, David; Mandelbaum, Rachel; Matsubara, Takahiko; McGehee, P.; McKay, Timothy A.; Meiksin, Avery; Munn, Jeffrey A.; Nakajima, Reiko; Nash, T.; Neilsen, Eric H.; Newberg, Heidi Jo; Newman, Peter R.; Nichol, R. C.; Nicinski, Tom; Nieto-Santisteban, María; Nitta, A.; O’Mullane, W.; Okamura, S.; Owen, Russell; Padmanabhan, Nikhil; Pauls, George; Peoples, J.; Pier, Jeffrey R.; Pope, Adrian; Pourbaix, D.; Quinn, Thomas; Richards, Gordon T.; Richmond, M.; Rockosi, Constance M.; Schlegel, David J.; Schneider, Donald P.; Schroeder, Joshua J.; Scranton, Ryan; Seljak, Uroš; Sheldon, E.; Shimasaku, K.; Smith, J. Allyn; Smolić, Vernesa; Snedden, Stephanie A.; Stoughton, Chris; Strauss, Michael A.; Rao, Mark Subba; Szalay, Alexander S.; Szapudi, István; Szkody, Paula; Tegmark, Max; Thakar, Aniruddha R.; Tucker, D. L.; Uomoto, Alan; Berk, D. E. vanden; Vandenberg, Jan; Vogeley, Michael S.; Voges, W.; Vogt, Nicole P.; Walkowicz, Lucianne M.; Weinberg, David H.; West, Andrew A.; White, Simon D. M.; Xu, Y.; Yanny, B.; Yocum, D. R.; York, Donald G.; Zehavi, Idit; Zibetti, S.; Zucker, D. B.

doi:10.1086/497917

Cited by 999 publications

(494 citation statements)

References 49 publications

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“…However, with no photometric information on the secondary it is equally likely to be a white dwarf (e.g., De Gennaro et al 2008). At the implied magnitude of V ∼ 30 mag chances of direct detection are essentially null, which is confirmed by the lack of any obvious 5 The fainter star's g, r, and i of (21.0, 19.6, 18.9) mag from the Sloan Digital Sky Survey (Adelman-McCarthy et al 2006) compare to magnitudes of (19.6, 18.6, 18.2) mag for Her-3. Also the Strömgren photometry of Adén et al (2009) identify it as a redder foreground dwarf.…”

Section: Musings On the Secondarymentioning

confidence: 99%

A Spectroscopic Binary in the Hercules Dwarf Spheroidal Galaxy

Koch

Hansen

Feltzing

et al. 2013

ApJ

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We present the radial velocity curve of a single-lined spectroscopic binary in the faint Hercules dwarf spheroidal (dSph) galaxy, based on 34 individual spectra covering more than 2 yr of observations. This is the first time that orbital elements could be derived for a binary in a dSph. The system consists of a metal-poor red giant and a low-mass companion, possibly a white dwarf, with a 135 day period in a moderately eccentric (e = 0.18) orbit. Its period and eccentricity are fully consistent with metal-poor binaries in the Galactic halo, while the projected semimajor axis is small, at a p sin i = 38 R . In fact, a very close orbit could inhibit the production of heavier elements through s-process nucleosynthesis, leading to the very low abundances of neutron-capture elements that are found in this star. We discuss the further implications for the chemical enrichment history of the Hercules dSph, but find no compelling binary scenario that could reasonably explain the full, peculiar abundance pattern of the Hercules dSph galaxy.

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Section: Musings On the Secondarymentioning

confidence: 99%

A Spectroscopic Binary in the Hercules Dwarf Spheroidal Galaxy

Koch

Hansen

Feltzing

et al. 2013

ApJ

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“…Here we briefly review the cluster redshift surveys and sources of the weak lensing profiles we compare with our dynamical estimates. Rines & Diaferio (2008) extracted the CIRS sample from the Fourth Data Release of the SDSS (Adelman-McCarthy et al 2006). The cluster sample is X-ray flux limited with f x > 3 × 10 −12 erg s −1 cm −2 (0.1-2.4 keV).…”

Section: Cluster Surveys and Weak Lensing Mass Profilesmentioning

confidence: 99%

Measuring the Mass Distribution in Galaxy Clusters

Geller

Diaferio

Rines

et al. 2013

ApJ

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Cluster mass profiles are tests of models of structure formation. Only two current observational methods of determining the mass profile, gravitational lensing, and the caustic technique are independent of the assumption of dynamical equilibrium. Both techniques enable the determination of the extended mass profile at radii beyond the virial radius. For 19 clusters, we compare the mass profile based on the caustic technique with weak lensing measurements taken from the literature. This comparison offers a test of systematic issues in both techniques. Around the virial radius, the two methods of mass estimation agree to within ∼30%, consistent with the expected errors in the individual techniques. At small radii, the caustic technique overestimates the mass as expected from numerical simulations. The ratio between the lensing profile and the caustic mass profile at these radii suggests that the weak lensing profiles are a good representation of the true mass profile. At radii larger than the virial radius, the extrapolated Navarro, Frenk & White fit to the lensing mass profile exceeds the caustic mass profile. Contamination of the lensing profile by unrelated structures within the lensing kernel may be an issue in some cases; we highlight the clusters MS0906+11 and A750, superposed along the line of sight, to illustrate the potential seriousness of contamination of the weak lensing signal by these unrelated structures.

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“…It was classified as a galaxy by the spectroscopic pipeline of the SDSS Fourth Data Release (Adelman-McCarthy et al 2006). In the course of our systematic spectral fitting of all extragalactic objects in the SDSS, we first noted UM 625 because it showed evident broad Hα and Hβ emission; its inferred virial BH mass placed it in the sample of type 1 AGNs with BH masses below 2 × 10 6 M described by Dong et al (2012b).…”

Section: Analysis Of the Optical Spectrummentioning

confidence: 99%

Um 625 Revisited: Multiwavelength Study of a Seyfert 1 Galaxy With a Low-Mass Black Hole

Jiang

Dong

et al. 2013

ApJ

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UM 625, previously identified as a narrow-line active galactic nucleus (AGN), actually exhibits broad Hα and Hβ lines whose width and luminosity indicate a low black hole (BH) mass of 1.6 × 10 6 M . We present a detailed multiwavelength study of the nuclear and host galaxy properties of UM 625. Analysis of Chandra and XMM-Newton observations suggests that this system contains a heavily absorbed and intrinsically X-ray weak (α ox = −1.72) nucleus. Although not strong enough to qualify as radio loud, UM 625 does belong to a minority of low-mass AGNs detected in the radio. The broadband spectral energy distribution constrains the bolometric luminosity to L bol ≈ (0.5-3) × 10 43 erg s −1 and L bol /L Edd ≈ 0.02-0.15. A comprehensive analysis of Sloan Digital Sky Survey and Hubble Space Telescope images shows that UM 625 is a nearly face-on S0 galaxy with a prominent, relatively blue pseudobulge (Sérsic index n = 1.60) that accounts for ∼60% of the total light in the R band. The extended disk is featureless, but the central ∼150-400 pc contains a conspicuous semi-ring of bright, blue star-forming knots, whose integrated ultraviolet luminosity suggests a star formation rate of ∼0.3 M yr −1 . The mass of the central BH roughly agrees with the value predicted from its bulge velocity dispersion but is significantly lower than that expected from its bulge luminosity.

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The Fourth Data Release of the Sloan Digital Sky Survey

Cited by 999 publications

References 49 publications

A Spectroscopic Binary in the Hercules Dwarf Spheroidal Galaxy

A Spectroscopic Binary in the Hercules Dwarf Spheroidal Galaxy

Measuring the Mass Distribution in Galaxy Clusters

Um 625 Revisited: Multiwavelength Study of a Seyfert 1 Galaxy With a Low-Mass Black Hole

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