The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data From SDSS-Iii

Alam, Shadab; Albareti, Franco D.; Prieto, C. Allende; Anders, F.; Anderson, Scott F.; Anderton, Timothy; Andrews, Brett H.; Armengaud, E.; Aubourg, É.; Bailey, S.; Basu, Sarbani; Bautista, Julian; Beaton, Rachael L.; Beers, Timothy C.; Bender, Chad F.; Berlind, Andreas A.; Beutler, Florian; Bhardwaj, Vaishali; Bird, Jonathan C.; Bizyaev, Dmitry; Blake, Cullen H.; Blanton, Michael R.; Blomqvist, Michael; Bochanski, John J.; Bolton, A.; Bovy, Jo; Bradley, A.; Brandt, W. N.; Brauer, D. E.; Brinkmann, J.; Brown, P. J.; Brownstein, Joel R.; Burden, A.; Burtin, E.; Busca, N. G.; Cai, Zheng; Capozzi, D.; Rosell, A. Carnero; Carr, Michael; Carrera, R.; Chambers, K.; Chaplin, W. J.; Chen, Yen‐Chi; Chiappini, Cristina; Chojnowski, S. Drew; Chuang, Chia-Hsun; Clerc, N.; Comparat, Johan; Covey, Kevin R.; Croft, Rupert A. C.; Cuesta, Antonio J.; Cunha, Kátia; Costa, L. N. da; Rio, Nicola Da; Davenport, James R. A.; Dawson, Kyle; Lee, Nathan De; Delubac, Timothée; Deshpande, Rohit; Dhital, Saurav; Dutra-Ferreira, Letícia; Dwelly, T.; Ealet, A.; Ebelke, Garrett; Edmondson, Edward M.; Eisenstein, Daniel J.; Ellsworth, Tristan; Elsworth, Y.; Epstein, Courtney R.; Eracleous, Michael; Escoffier, S.; Esposito, M.; Evans, Michael L.; Fan, Xiaohui; Fernández-Alvar, Emma; Feuillet, Diane; Ak, N. Filiz; Finley, Hayley; Finoguenov, A.; Flaherty, Kevin; Fleming, Scott W.; Font-Ribera, Andreu; Foster, Jonathan B.; Frinchaboy, Peter M.; Galbraith-Frew, Jessica; García, Rafael A.; García-Hernández, D. A.; Pérez, Ana E. García; Gaulme, P.; Ge, Jian; Génova-Santos, R. T.; Georgakakis, A.; Ghezzi, Luan; Gillespie, Bruce; Girardi, L.; Goddard, Daniel; Gontcho, Satya Gontcho A; Hernández, J. I. González; Grebel, Eva K.; Green, Paul; Grieb, Jan Niklas; Grieves, Nolan; Gunn, James E.; Guo, Hong; Harding, Paul; Hasselquist, Sten; Hawley, Suzanne L.; Hayden, Michael R.; Hearty, Fred; Hekker, S.; Ho, Shirley; Hogg, David W.; Holley‐Bockelmann, Kelly; Holtzman, Jon A.; Honscheid, K.; Huber, Daniel; Huehnerhoff, Joseph; Ivans, Inese I.; Jiang, Linhua; Johnson, Jennifer A.; Kinemuchi, Karen; Kirkby, D.; Kitaura, Francisco-Shu; Klaene, Mark A.; Knapp, G. R.; Kneib, Jean-Paul; Koenig, X.; Lam, Charles R.; Lan, Ting-Wen; Lang, Dustin; Laurent, Pierre; Goff, Jean-Marc Le; Leauthaud, Alexie; Lee, Khee-Gan; Lee, Young Sun; Licquia, Timothy C.; Liu, Jian; Long, Daniel C.; López-Corredoira, Martín; Lorenzo-Oliveira, Diego; Lucatello, S.; Lundgren, Britt; Lupton, Robert H.; Mack, Claude E.; Mahadevan, Suvrath; Maia, M. A. G.; Majewski, Steven R.; Malanushenko, Elena; Malanushenko, Viktor; Manchado, A.; Manera, Marc; Mao, Qingqing; Maraston, Claudia; Marchwinski, Robert C.; Margala, Daniel; Martell, Sarah L.; Martig, Marie; Masters, Karen L.; Mathur, S.; McBride, Cameron K.; McGehee, P.; McGreer, Ian D.; McMahon, R. G.; Ménard, Brice; Menzel, Marie-Luise; Merloni, A.; Mészáros, Szabolcs; Miller, A. A.; Miralda-Escudé, Jordi; Miyatake, Hironao; Montero-Dorta, Antonio D.; More, Surhud; Morganson, E.; Morice-Atkinson, Xan; Morrison, Heather; Mosser, B.; Muna, Demitri; Myers, Adam D.; Nandra, K.; Newman, Jeffrey A.; Neyrinck, Mark C.; Nguyen, Duy Cuong; Nichol, R. C.; Nidever, David L.; Noterdaeme, P.; Nuza, Sebastián E.; O’Connell, Julia; O’Connell, R. W.; O’Connell, Ross; Ogando, R. L. C.; Olmstead, Matthew D.; Oravetz, Audrey; Oravetz, Daniel; Osumi, Keisuke; Owen, Russell; Padgett, Deborah; Padmanabhan, Nikhil; Paegert, Martin; Palanque-Delabrouille, N.; Pan, Kaike; Parejko, John K.; Pâris, Isabelle; Park, Changbom; Pattarakijwanich, P.; Pellejero-Ibáñez, Marcos; Pepper, Joshua; Percival, Will J.; Pérez-Fournón, I.; ́rez-Ra`fols, Ignasi Pe; Petitjean, P.; Pieri, Matthew M.; Pinsonneault, Marc H.; Mello, G. F. Porto de; Prada, Francisco; Prakash, Abhishek; Price-Whelan, Adrian M.; Protopapas, Pavlos; Raddick, M. Jordan; Rahman, Mubdi; Reid, Beth; Rich, J.; Rix, Hans─Walter; Robin, A. C.; Rockosi, Constance M.; Rodrigues, Thaíse S.; Rodríguez-Torres, Sergio; Roe, Natalie A.; Ross, Ashley J.; Ross, Nicholas P.; Rossi, Graziano; Ruan, John J.; Rubiño-Martín, J. A.; Rykoff, E. S.; Salazar-Albornoz, Salvador; Salvato, M.; Samushia, Lado; Sánchez, Ariel G.; Santiago, B.; Sayres, Conor; Schiavon, Ricardo P.; Schlegel, David J.; Schmidt, Sarah J.; Schneider, Donald P.; Schultheis, M.; Schwope, A. D.; Scóccola, Claudia G.; Scott, Caroline; Sellgren, K.; Seo, Hee-Jong; Serenelli, Aldo; Shane, N.; Shen, Yue; Shetrone, Matthew; Shu, Y.; Aguirre, V. Silva; Sivarani, T.; Skrutskie, Michael F.; Slosar, Anže; Smith, Verne V.; Sobreira, F.; Souto, Diogo; Stassun, Keivan G.; Steinmetz, Matthias; Stello, Dennis; Strauss, Michael A.; Streblyanska, A.; Suzuki, N.; Swanson, M. E. C.; Tan, Jonathan C.; Tayar, Jamie; Terrien, Ryan C.; Thakar, Aniruddha R.; Thomas, Daniel; Thomas, Neil; Thompson, Benjamin; Tinker, Jeremy L.; Tojeiro, Rita; Troup, Nicholas; Vargas-Magaña, Mariana; Vázquez, J. Alberto; Verde, Licia; Viel, Matteo; Vogt, Nicole P.; Wake, David A.; Wang, Ji; Weaver, B. A.; Weinberg, David H.; Weiner, Benjamin J.; White, Martin; Wilson, John C.; Wisniewski, John P.; Wood‐Vasey, W. M.; Yèche, Ch; York, Donald G.; Zakamska, Nadia L.; Zamora, Olga; Zasowski, Gail; Zehavi, Idit; Zhao, Gong-Bo; Zhang, Zheng; Xu, Zhiyong; Zhang, Zhimin; Zou, Hu; Zhu, Guangtun

doi:10.1088/0067-0049/219/1/12

Cited by 2,257 publications

(1,382 citation statements)

References 137 publications

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“…As we based the definition of the average ∆ν for MESA models similar to the one used in Handberg et al (2016)'s work, we adopted their values for the global seismic (∆ν and νmax) and spectroscopic (T eff ) parameters. We verified that their T eff scale is just ∼ 57 K cooler than the spectroscopic measurements from the APOGEE Data Release 12 (Alam et al 2015). The metallicity adopted was [Fe/H] = 0.02 ± 0.10 dex for all stars.…”

Section: Ngc 6819supporting

confidence: 55%

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Rodrigues

Bossini

Miglio

et al. 2017

Mon. Not. R. Astron. Soc.

Self Cite

103

119

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Asteroseismic parameters allow us to measure the basic stellar properties of field giants observed far across the Galaxy. Most of such determinations are, up to now, based on simple scaling relations involving the large frequency separation, ∆ν, and the frequency of maximum power, ν max . In this work, we implement ∆ν and the period spacing, ∆P , computed along detailed grids of stellar evolutionary tracks, into stellar isochrones and hence in a Bayesian method of parameter estimation. Tests with synthetic data reveal that masses and ages can be determined with typical precision of 5 and 19 per cent, respectively, provided precise seismic parameters are available. Adding independent information on the stellar luminosity, these values can decrease down to 3 and 10 per cent respectively. The application of these methods to NGC 6819 giants produces a mean age in agreement with those derived from isochrone fitting, and no evidence of systematic differences between RGB and RC stars. The age dispersion of NGC 6819 stars, however, is larger than expected, with at least part of the spread ascribable to stars that underwent mass-transfer events.

show abstract

Section: Ngc 6819supporting

confidence: 55%

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Rodrigues

Bossini

Miglio

et al. 2017

Mon. Not. R. Astron. Soc.

Self Cite

103

119

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show abstract

“…As described below, our study is based on an unprecedentedly large sample of ∼ 38,000 LRGs spectroscopically identified at projected distances of d < 500 kpc from the sightline of a background QSO. Both LRGs and the background QSOs are found in the SDSS spectroscopic catalog from DR12 (Alam et al 2015). While the signal-to-noise (S/N ) of the QSO spectra varies according to the apparent brightnesses of the QSOs, we are able to constrain the presence/absence of Mg II absorbers with rest-frame absorption equivalent width Wr(2796) 0.3 A for 35% of the total LRG sample.…”

Section: Introductionmentioning

confidence: 95%

“…We first considered the galaxies and quasars from the Data Release (DR12, Alam et al 2015) of SDSS, particularly those in the Baryon Oscillation Spectroscopic Survey (BOSS, Dawson et al 2013). In total, imaging and spectroscopic data were obtained in BOSS for ∼ 1.5 million luminous galaxies at mean redshift z ≈ 0.6.…”

Section: The Lrg-qso Pair Catalogmentioning

confidence: 99%

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Huang

Chen

Johnson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We report a definitive detection of chemically-enriched cool gas around massive, quiescent galaxies at z ≈ 0.4 − 0.7. The result is based on a survey of 37621 luminous red galaxy (LRG)-QSO pairs in SDSS DR12 with projected distance d < 500 kpc. LRGs at d < 50 kpc, provides important insights into the origin of the observed chemically-enriched cool gas in LRG halos. We consider different scenarios and conclude that the observed Mg II absorbers around LRGs are best-explained by a combination of cool clouds formed in thermally unstable LRG halos and satellite accretion through filaments.

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“…In this work, we use the second release of value-added catalogues of LSS-GAC (LSS-GAC DR2; Xiang et al 2016, in preparation), the ninth SDSS/SEGUE public data release (SDSS/SEGUE DR9; Ahn et al 2012) and the twelfth SDSS-III/APOGEE public data release (SDSS-III/APOGEE DR12; Alam et al 2015).…”

Section: Lss-gac Sdss/segue and Sdss-iii/apogee Datamentioning

confidence: 99%

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Huang

Liu

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

165

179

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The rotation curve (RC) of the Milky Way out to ∼ 100 kpc has been constructed using ∼ 16, 000 primary red clump giants (PRCGs) in the outer disk selected from the LSS-GAC and the SDSS-III/APOGEE survey, combined with ∼ 5700 halo K giants (HKGs) selected from the SDSS/SEGUE survey. To derive the RC, the PRCG sample of the warm disc population and the HKG sample of halo stellar population are respectively analyzed using a kinematical model allowing for the asymmetric drift corrections and re-analyzed using the spherical Jeans equation along with measurements of the anisotropic parameter β currently available. The typical uncertainties of RC derived from the PRCG and HKG samples are respectively 5-7 km s −1 and several tens km s −1 . We determine a circular velocity at the solar position, V c (R 0 ) = 240 ± 6 km s −1 and an azimuthal peculiar speed of the Sun, V ⊙ = 12.1 ± 7.6 km s −1 , both in good agreement with the previous determinations. The newly constructed RC has a generally flat value of 240 km s −1 within a Galactocentric distance r of 25 kpc and then decreases steadily to 150 km s −1 at r ∼ 100 kpc. On top of this overall trend, the RC exhibits two prominent localized dips, one at r ∼ 11 kpc and another at r ∼ 19 kpc. From the newly constructed RC, combined with other constraints, we have built a parametrized mass model for the Galaxy, yielding a virial mass of the Milky Way's dark matter halo of 0.90 +0.07 −0.08 × 10 12 M ⊙ and a local dark matter density, ρ ⊙,dm = 0.32 +0.02 −0.02 GeV cm −3 .

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The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data From SDSS-Iii

Cited by 2,257 publications

References 137 publications

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

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