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1. Lithium Isotopic Abundances in Old Stars

Author

García Pérez, Ana Elia, Inoue, Susumu, Aoki, Wako, Ryan, Sean, Leibundgut, Bruno, editor, Santos, Nuno C., editor, Pasquini, Luca, editor, Correia, Alexandre C. M., editor, and Romaniello, Martino, editor

Published
2008
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2. Bayesian distances and extinctions for giants observed by Kepler and APOGEE

Author

Rodrigues, Thaise da Silva, Girardi, Leo Alberto, Miglio, Andrea, Bossini, Diego, Bovy, Jo, Epstein, Courtney, Pinsonneault, Marc H., Zasowski, G., Allende Prieto, Carlos, Chaplin, William James, Hekker, Saskia, Johnson, J.A., Mészáros, S., Mosser, Benoît, Anders, Friedrich, Basu, Sarbani, Beers, T.C., Chiappini, C.C.M., Costa, Luiz N. da, Elsworth, Yvonne P., Garcia, Rafael A., García Pérez, Ana Elia, Maia, Marcio Antonio Geimba, Majewski, Steven Raymond, Mathur, Savita, Montalbán, Josefina, Nidever, D.L., Santiago, Basilio Xavier, Schultheis, Mathias, Serenelli, Aldo M., and Shetrone, M.

Subjects
Evolucao estelar, Aglomerados estelares, Catalogos astronomicos, Estrelas gigantes, distances [Stars], fundamental parameters [Stars]
Abstract

We present a first determination of distances and extinctions for individual stars in the first release of the APOKASC catalogue, built from the joint efforts of the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and the Kepler Asteroseismic Science Consortium (KASC). Our method takes into account the spectroscopic constraints derived from the APOGEE Stellar Parameters and Chemical Abundances Pipeline, together with the asteroseismic parameters from KASC. These parameters are then employed to estimate intrinsic stellar properties, including absolute magnitudes, using the Bayesian tool PARAM. We then find the distance and extinction that best fit the observed photometry in Sloan Digital Sky Survey (SDSS), 2MASS, and WISE passbands. The first 1989 giants targetted by APOKASC are found at typical distances between 0.5 and 5 kpc, with individual uncertainties of just ∼1.8 per cent. Our extinction estimates are systematically smaller than provided in the Kepler Input Catalogue and by the Schlegel et al. maps. Distances to individual stars in the NGC 6791 and NGC 6819 star clusters agree to within their credible intervals. Comparison with the APOGEE red clump and SAGA catalogues provide another useful check, exhibiting agreement with our measurements to within a few per cent. Overall, present methods seem to provide excellent distance and extinction determinations for the bulk of the APOKASC sample. Approximately one third of the stars present broad or multiple-peaked probability density functions and hence increased uncertainties. Uncertainties are expected to be reduced in future releases of the catalogue, when a larger fraction of the stars will have seismically determined evolutionary status classifications.

Published
2014

3. THE APOGEE SPECTROSCOPIC SURVEY OFKEPLERPLANET HOSTS: FEASIBILITY, EFFICIENCY, AND FIRST RESULTS

Author

Fleming, Scott W., primary, Mahadevan, Suvrath, additional, Deshpande, Rohit, additional, Bender, Chad F., additional, Terrien, Ryan C., additional, Marchwinski, Robert C., additional, Wang, Ji, additional, Roy, Arpita, additional, Stassun, Keivan G., additional, Prieto, Carlos Allende, additional, Cunha, Katia, additional, Smith, Verne V., additional, Agol, Eric, additional, Ak, Hasan, additional, Bastien, Fabienne A., additional, Bizyaev, Dmitry, additional, Crepp, Justin R., additional, Ford, Eric B., additional, Frinchaboy, Peter M., additional, García-Hernández, Domingo Aníbal, additional, García Pérez, Ana Elia, additional, Gaudi, B. Scott, additional, Ge, Jian, additional, Hearty, Fred, additional, Ma, Bo, additional, Majewski, Steve R., additional, Mészáros, Szabolcs, additional, Nidever, David L., additional, Pan, Kaike, additional, Pepper, Joshua, additional, Pinsonneault, Marc H., additional, Schiavon, Ricardo P., additional, Schneider, Donald P., additional, Wilson, John C., additional, Zamora, Olga, additional, and Zasowski, Gail, additional

Published
2015
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4. On the Abundances of Li, Be and O in Metal-Poor Stars in the Galaxy

Author

García Pérez, Ana Elia

Subjects
stellar abundances, stellar mixing, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomi och astrofysik, Astronomi, astrofysik och kosmologi, Astronomy and astrophysics, Astronomi, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, galactic evolution, Astrophysics::Earth and Planetary Astrophysics, spectral line formation, Astrophysics::Galaxy Astrophysics, stellar atmospheres
Abstract

Stellar atmospheres constitute excellent environments to study the chemical evolution of our Galaxy. The chemical composition of these atmospheres reflects the composition of the gas from where these stars were born. As the Galaxy evolves, the composition of the gas changes from being primordial (Big-Bang nucleosynthesis) to being enriched in heavy elements (stellar and interstellar nucleosynthesis). The abundances of fragile chemical elements can be affected by stellar mixing processes. Precise lithium, beryllium and oxygen abundance determinations in old stars are presented in this thesis. These determinations are based on the analysis of the observed spectra of a sample of thirteen metal-poor subgiant stars. According to stellar mixing theories, these stars are in a stellar evolutionary stage in which mixing by convection is expected. Abundances of fragile elements like lithium and beryllium are thus expected to be affected by such mixing processes. As a consequence of this, the abundances of these elements are discussed in a dilution context. Lithium and beryllium abundances are compared with the abundances of stars with similar characteristics but in a less evolved stellar phase so that mixing processes have not acted yet. As expected, our abundances seem to be depleted following reasonably well the standard predictions. Stellar abundances of oxygen should give an estimate of the oxygen contribution of core-collapse supernovae to the interstellar medium. However, there is poor agreement among the abundances determined from different atomic or molecular indicators in general. Abundances coming from three different indicators are compared in this thesis. The abundances determined from the O I infrared triplet lines at 777.1-5 nm give the poorest agreement among the three indicators. The abundances based on OH ultraviolet lines around 310 nm are lower for the subgiants in comparison with previous studies of main-sequence stars, becoming even lower than values based on the O I forbidden line at 630.03 nm. Still the most reliable indicator appears to be the O I forbidden line which suggests a plateau-like or only slowly increasing [O/Fe] towards lower [Fe/H]. In addition, the line formation of the Be II ultraviolet resonance lines at 313.0-1 nm, commonly used for abundance determinations purposes, is investigated under non-local thermodynamic equilibrium. We find that the common assumption of local thermodynamic equilibrium typically gives systematic errors of about 0.1 dex.

Published
2005

6. THE OPEN CLUSTER CHEMICAL ANALYSIS AND MAPPING SURVEY: LOCAL GALACTIC METALLICITY GRADIENT WITH APOGEE USING SDSS DR10

Author

Frinchaboy, Peter M., primary, Thompson, Benjamin, additional, Jackson, Kelly M., additional, O'Connell, Julia, additional, Meyer, Brianne, additional, Zasowski, Gail, additional, Majewski, Steven R., additional, Chojnowksi, S. Drew, additional, Johnson, Jennifer A., additional, Allende Prieto, Carlos, additional, Beers, Timothy C., additional, Bizyaev, Dmitry, additional, Brewington, Howard, additional, Cunha, Katia, additional, Ebelke, Garrett, additional, García Pérez, Ana Elia, additional, Hearty, Frederick R., additional, Holtzman, Jon, additional, Kinemuchi, Karen, additional, Malanushenko, Elena, additional, Malanushenko, Viktor, additional, Marchante, Moses, additional, Mészáros, Szabolcs, additional, Muna, Demitri, additional, Nidever, David L., additional, Oravetz, Daniel, additional, Pan, Kaike, additional, Schiavon, Ricardo P., additional, Schneider, Donald P., additional, Shetrone, Matthew, additional, Simmons, Audrey, additional, Snedden, Stephanie, additional, Smith, Verne V., additional, and Wilson, John C., additional

Published
2013
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7. Oxygen abundances in metal-poor subgiants as determined from [OI], OI and OH lines

Author

García Pérez, Ana Elia, Asplund, Martin, Primas, Francesca, Nissen, Poul Erik, Gustafsson, Bengt, García Pérez, Ana Elia, Asplund, Martin, Primas, Francesca, Nissen, Poul Erik, and Gustafsson, Bengt

Abstract

The debate on the oxygen abundances of metal-poor stars has its origin in contradictory results obtained using different abundance indicators. To achieve a better understanding of the problem we have acquired high quality spectra with the Ultraviolet and Visual Echelle Spectrograph at VLT, with a signal-to-noise of the order of 100 in the near ultraviolet and 500 in the optical and near infrared wavelength range. Three different oxygen abundance indicators, OH ultraviolet lines around 310.0 nm, the [O I] line at 630.03 nm and the O I lines at 777.1-5 nm were observed in the spectra of 13 metal-poor subgiants with . Oxygen abundances were obtained from the analysis of these indicators which was carried out assuming local thermodynamic equilibrium and plane-parallel model atmospheres. Abundances derived from O I were corrected for departures from local thermodynamic equilibrium. Stellar parameters were computed using -vs.-color calibrations based on the infrared flux method and Balmer line profiles, Hipparcos parallaxes and lines. [O/Fe] values derived from the forbidden line at 630.03 nm are consistent with an oxygen/iron ratio that varies linearly with [Fe/H] as . Values based on the O I triplet are on average (s.d.) higher than the values based on the forbidden line while the agreement between OH ultraviolet lines and the forbidden line is much better with a mean difference of the order of (s.d.). In general, our results follow the same trend as previously published results with the exception of the ones based on OH ultraviolet lines. In that case our results lie below the values which gave rise to the oxygen abundance debate for metal-poor stars.

Published
2006
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8. Li and Be depletion in metal-poor subgiants

Author

García Pérez, Ana Elia, Primas, Francesca, García Pérez, Ana Elia, and Primas, Francesca

Abstract

A sample of metal-poor subgiants has been observed with the UVES spectrograph at the Very Large Telescope and abundances of Li and Be have been determined. Typical signal-to-noise per spectral bin values for the co-added spectra are of the order of 500 for the line (670.78 nm) and 100 for the doublet lines (313.04 nm). The spectral analysis of the observations was carried out using the Uppsala suite of codes and MARCS (1D-LTE) model atmospheres with stellar parameters from photometry, parallaxes, isochrones and Fe II lines. Abundance estimates of the light elements were corrected for departures from local thermodynamic equilibrium in the line formation. Effective temperatures and Li abundances seem to be correlated and Be abundances correlate with [O/H]. Standard models predict Li and Be abundances approximately one order of magnitude lower than main-sequence values which is in general agreement with the observations. On average, our observed depletions seem to be 0.1 dex smaller and between 0.2 and 0.4 dex larger (depending on which reference is taken) than those predicted for Li and Be, respectively. This is not surprising since the initial Li abundance, as derived from main-sequence stars on the Spite plateau, may be systematically in error by 0.1 dex or more, and uncertainties in the spectrum normalisation and continuum drawing may affect our Be abundances systematically.

Published
2006
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9. THE MILKY WAY'S CIRCULAR-VELOCITY CURVE BETWEEN 4 AND 14 kpc FROM APOGEE DATA

Author

Bovy, Jo, primary, Allende Prieto, Carlos, additional, Beers, Timothy C., additional, Bizyaev, Dmitry, additional, da Costa, Luiz N., additional, Cunha, Katia, additional, Ebelke, Garrett L., additional, Eisenstein, Daniel J., additional, Frinchaboy, Peter M., additional, García Pérez, Ana Elia, additional, Girardi, Léo, additional, Hearty, Fred R., additional, Hogg, David W., additional, Holtzman, Jon, additional, Maia, Marcio A. G., additional, Majewski, Steven R., additional, Malanushenko, Elena, additional, Malanushenko, Viktor, additional, Mészáros, Szabolcs, additional, Nidever, David L., additional, O'Connell, Robert W., additional, O'Donnell, Christine, additional, Oravetz, Audrey, additional, Pan, Kaike, additional, Rocha-Pinto, Helio J., additional, Schiavon, Ricardo P., additional, Schneider, Donald P., additional, Schultheis, Mathias, additional, Skrutskie, Michael, additional, Smith, Verne V., additional, Weinberg, David H., additional, Wilson, John C., additional, and Zasowski, Gail, additional

Published
2012
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10. THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT: FIRST DETECTION OF HIGH-VELOCITY MILKY WAY BAR STARS

Author

Nidever, David L., primary, Zasowski, Gail, additional, Majewski, Steven R., additional, Bird, Jonathan, additional, Robin, Annie C., additional, Martinez-Valpuesta, Inma, additional, Beaton, Rachael L., additional, Schönrich, Ralph, additional, Schultheis, Mathias, additional, Wilson, John C., additional, Skrutskie, Michael F., additional, O’Connell, Robert W., additional, Shetrone, Matthew, additional, Schiavon, Ricardo P., additional, Johnson, Jennifer A., additional, Weiner, Benjamin, additional, Gerhard, Ortwin, additional, Schneider, Donald P., additional, Allende Prieto, Carlos, additional, Sellgren, Kris, additional, Bizyaev, Dmitry, additional, Brewington, Howard, additional, Brinkmann, Jon, additional, Eisenstein, Daniel J., additional, Frinchaboy, Peter M., additional, García Pérez, Ana Elia, additional, Holtzman, Jon, additional, Hearty, Fred R., additional, Malanushenko, Elena, additional, Malanushenko, Viktor, additional, Muna, Demitri, additional, Oravetz, Daniel, additional, Pan, Kaike, additional, Simmons, Audrey, additional, Snedden, Stephanie, additional, and Weaver, Benjamin A., additional

Published
2012
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11. SDSS-III: MASSIVE SPECTROSCOPIC SURVEYS OF THE DISTANT UNIVERSE, THE MILKY WAY, AND EXTRA-SOLAR PLANETARY SYSTEMS

Author

Eisenstein, Daniel J., primary, Weinberg, David H., additional, Agol, Eric, additional, Aihara, Hiroaki, additional, Allende Prieto, Carlos, additional, Anderson, Scott F., additional, Arns, James A., additional, Aubourg, Éric, additional, Bailey, Stephen, additional, Balbinot, Eduardo, additional, Barkhouser, Robert, additional, Beers, Timothy C., additional, Berlind, Andreas A., additional, Bickerton, Steven J., additional, Bizyaev, Dmitry, additional, Blanton, Michael R., additional, Bochanski, John J., additional, Bolton, Adam S., additional, Bosman, Casey T., additional, Bovy, Jo, additional, Brandt, W. N., additional, Breslauer, Ben, additional, Brewington, Howard J., additional, Brinkmann, J., additional, Brown, Peter J., additional, Brownstein, Joel R., additional, Burger, Dan, additional, Busca, Nicolas G., additional, Campbell, Heather, additional, Cargile, Phillip A., additional, Carithers, William C., additional, Carlberg, Joleen K., additional, Carr, Michael A., additional, Chang, Liang, additional, Chen, Yanmei, additional, Chiappini, Cristina, additional, Comparat, Johan, additional, Connolly, Natalia, additional, Cortes, Marina, additional, Croft, Rupert A. C., additional, Cunha, Katia, additional, da Costa, Luiz N., additional, Davenport, James R. A., additional, Dawson, Kyle, additional, De Lee, Nathan, additional, Porto de Mello, Gustavo F., additional, de Simoni, Fernando, additional, Dean, Janice, additional, Dhital, Saurav, additional, Ealet, Anne, additional, Ebelke, Garrett L., additional, Edmondson, Edward M., additional, Eiting, Jacob M., additional, Escoffier, Stephanie, additional, Esposito, Massimiliano, additional, Evans, Michael L., additional, Fan, Xiaohui, additional, Femenía Castellá, Bruno, additional, Dutra Ferreira, Leticia, additional, Fitzgerald, Greg, additional, Fleming, Scott W., additional, Font-Ribera, Andreu, additional, Ford, Eric B., additional, Frinchaboy, Peter M., additional, García Pérez, Ana Elia, additional, Gaudi, B. Scott, additional, Ge, Jian, additional, Ghezzi, Luan, additional, Gillespie, Bruce A., additional, Gilmore, G., additional, Girardi, Léo, additional, Gott, J. Richard, additional, Gould, Andrew, additional, Grebel, Eva K., additional, Gunn, James E., additional, Hamilton, Jean-Christophe, additional, Harding, Paul, additional, Harris, David W., additional, Hawley, Suzanne L., additional, Hearty, Frederick R., additional, Hennawi, Joseph F., additional, González Hernández, Jonay I., additional, Ho, Shirley, additional, Hogg, David W., additional, Holtzman, Jon A., additional, Honscheid, Klaus, additional, Inada, Naohisa, additional, Ivans, Inese I., additional, Jiang, Linhua, additional, Jiang, Peng, additional, Johnson, Jennifer A., additional, Jordan, Cathy, additional, Jordan, Wendell P., additional, Kauffmann, Guinevere, additional, Kazin, Eyal, additional, Kirkby, David, additional, Klaene, Mark A., additional, Knapp, G. R., additional, Kneib, Jean-Paul, additional, Kochanek, C. S., additional, Koesterke, Lars, additional, Kollmeier, Juna A., additional, Kron, Richard G., additional, Lampeitl, Hubert, additional, Lang, Dustin, additional, Lawler, James E., additional, Le Goff, Jean-Marc, additional, Lee, Brian L., additional, Lee, Young Sun, additional, Leisenring, Jarron M., additional, Lin, Yen-Ting, additional, Liu, Jian, additional, Long, Daniel C., additional, Loomis, Craig P., additional, Lucatello, Sara, additional, Lundgren, Britt, additional, Lupton, Robert H., additional, Ma, Bo, additional, Ma, Zhibo, additional, MacDonald, Nicholas, additional, Mack, Claude, additional, Mahadevan, Suvrath, additional, Maia, Marcio A. G., additional, Majewski, Steven R., additional, Makler, Martin, additional, Malanushenko, Elena, additional, Malanushenko, Viktor, additional, Mandelbaum, Rachel, additional, Maraston, Claudia, additional, Margala, Daniel, additional, Maseman, Paul, additional, Masters, Karen L., additional, McBride, Cameron K., additional, McDonald, Patrick, additional, McGreer, Ian D., additional, McMahon, Richard G., additional, Mena Requejo, Olga, additional, Ménard, Brice, additional, Miralda-Escudé, Jordi, additional, Morrison, Heather L., additional, Mullally, Fergal, additional, Muna, Demitri, additional, Murayama, Hitoshi, additional, Myers, Adam D., additional, Naugle, Tracy, additional, Neto, Angelo Fausti, additional, Nguyen, Duy Cuong, additional, Nichol, Robert C., additional, Nidever, David L., additional, O’Connell, Robert W., additional, Ogando, Ricardo L. C., additional, Olmstead, Matthew D., additional, Oravetz, Daniel J., additional, Padmanabhan, Nikhil, additional, Paegert, Martin, additional, Palanque-Delabrouille, Nathalie, additional, Pan, Kaike, additional, Pandey, Parul, additional, Parejko, John K., additional, Pâris, Isabelle, additional, Pellegrini, Paulo, additional, Pepper, Joshua, additional, Percival, Will J., additional, Petitjean, Patrick, additional, Pfaffenberger, Robert, additional, Pforr, Janine, additional, Phleps, Stefanie, additional, Pichon, Christophe, additional, Pieri, Matthew M., additional, Prada, Francisco, additional, Price-Whelan, Adrian M., additional, Raddick, M. Jordan, additional, Ramos, Beatriz H. F., additional, Reid, I. Neill, additional, Reyle, Celine, additional, Rich, James, additional, Richards, Gordon T., additional, Rieke, George H., additional, Rieke, Marcia J., additional, Rix, Hans-Walter, additional, Robin, Annie C., additional, Rocha-Pinto, Helio J., additional, Rockosi, Constance M., additional, Roe, Natalie A., additional, Rollinde, Emmanuel, additional, Ross, Ashley J., additional, Ross, Nicholas P., additional, Rossetto, Bruno, additional, Sánchez, Ariel G., additional, Santiago, Basilio, additional, Sayres, Conor, additional, Schiavon, Ricardo, additional, Schlegel, David J., additional, Schlesinger, Katharine J., additional, Schmidt, Sarah J., additional, Schneider, Donald P., additional, Sellgren, Kris, additional, Shelden, Alaina, additional, Sheldon, Erin, additional, Shetrone, Matthew, additional, Shu, Yiping, additional, Silverman, John D., additional, Simmerer, Jennifer, additional, Simmons, Audrey E., additional, Sivarani, Thirupathi, additional, Skrutskie, M. F., additional, Slosar, Anže, additional, Smee, Stephen, additional, Smith, Verne V., additional, Snedden, Stephanie A., additional, Stassun, Keivan G., additional, Steele, Oliver, additional, Steinmetz, Matthias, additional, Stockett, Mark H., additional, Stollberg, Todd, additional, Strauss, Michael A., additional, Szalay, Alexander S., additional, Tanaka, Masayuki, additional, Thakar, Aniruddha R., additional, Thomas, Daniel, additional, Tinker, Jeremy L., additional, Tofflemire, Benjamin M., additional, Tojeiro, Rita, additional, Tremonti, Christy A., additional, Vargas Magaña, Mariana, additional, Verde, Licia, additional, Vogt, Nicole P., additional, Wake, David A., additional, Wan, Xiaoke, additional, Wang, Ji, additional, Weaver, Benjamin A., additional, White, Martin, additional, White, Simon D. M., additional, Wilson, John C., additional, Wisniewski, John P., additional, Wood-Vasey, W. Michael, additional, Yanny, Brian, additional, Yasuda, Naoki, additional, Yèche, Christophe, additional, York, Donald G., additional, Young, Erick, additional, Zasowski, Gail, additional, Zehavi, Idit, additional, and Zhao, Bo, additional

Published
2011
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12. Lithium Isotopic Abundances in Old Stars.

Author

Leibundgut, Bruno, Santos, Nuno C., Pasquini, Luca, Correia, Alexandre C. M., Romaniello, Martino, García Pérez, Ana Elia, Inoue, Susumu, Aoki, Wako, and Ryan, Sean

Abstract

Lithium is an element of great importance from a cosmological point of view. Observations of its light isotope 6Li are very delicate and in the literature, detections for only a handful of metal-poor stars are found. High quality spectra (S/N∼450, R∼100000) of the Li i 670.8 nm resonance line of six metal-poor stars, taken at the Subaru telescope, are being analysed. The results based on the still early stage of the analysis suggest one possible detection and four possible upper limits (including the two most metal-poor stars in the sample) for 6Li. The observed spectra of the remaining star suggest that there is very little 6Li, if any at all. [ABSTRACT FROM AUTHOR]

Published
2008
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13. SDSS-III: massive spectroscopic surveys of the distant universe, the Milky Way, and extra-solar planetary systems

Author

Eisenstein, Daniel J., Weinberg, David H., Agol, Eric, Aihara, Hiroaki, Allende Prieto, Carlos, Anderson, Scott F., Arns, James A., Aubourg, Éric, Bailey, Stephen, Balbinot, Eduardo, Barkhouser, Robert, Beers, Timothy C., Berlind, Andreas A., Bickerton, Steven J., Bizyaev, Dmitry, Blanton, Michael R., Bochanski, John J., Bolton, Adam S., Bosman, Casey T., Bovy, Jo, Brandt, W. N., Breslauer, Ben, Brewington, Howard J., Brinkmann, J., Brown, Peter J., Brownstein, Joel R., Burger, Dan, Busca, Nicolas G., Campbell, Heather, Cargile, Phillip A., Carithers, William C., Carlberg, Joleen K., Carr, Michael A., Chang, Liang, Chen, Yanmei, Chiappini, Cristina, Comparat, Johan, Connolly, Natalia, Cortes, Marina, Croft, Rupert A. C., Cunha, Katia, da Costa, Luiz N., Davenport, James R. A., Dawson, Kyle, De Lee, Nathan, Porto de Mello, Gustavo F., de Simoni, Fernando, Dean, Janice, Dhital, Saurav, Ealet, Anne, Ebelke, Garrett L., Edmondson, Edward M., Eiting, Jacob M., Escoffier, Stephanie, Esposito, Massimiliano, Evans, Michael L., Fan, Xiaohui, Femenía Castellá, Bruno, Dutra Ferreira, Leticia, Fitzgerald, Greg, Fleming, Scott W., Font-Ribera, Andreu, Ford, Eric B., Frinchaboy, Peter M., García Pérez, Ana Elia, Gaudi, B. Scott, Ge, Jian, Ghezzi, Luan, Gillespie, Bruce A., Gilmore, G., Girardi, Léo, Gott, J. Richard, Gould, Andrew, Grebel, Eva K., Gunn, James E., Hamilton, Jean-Christophe, Harding, Paul, Harris, David W., Hawley, Suzanne L., Hearty, Frederick R., Hennawi, Joseph F., González Hernández, Jonay I., Ho, Shirley, Hogg, David W., Holtzman, Jon A., Honscheid, Klaus, Inada, Naohisa, Ivans, Inese I., Jiang, Linhua, Jiang, Peng, Johnson, Jennifer A., Jordan, Cathy, Jordan, Wendell P., Kauffmann, Guinevere, Kazin, Eyal, Kirkby, David, Klaene, Mark A., Knapp, G. R., Kneib, Jean-Paul, Kochanek, C. S., Koesterke, Lars, Kollmeier, Juna A., Kron, Richard G., Lampeitl, Hubert, Lang, Dustin, Lawler, James E., Le Goff, Jean-Marc, Lee, Brian L., Lee, Young Sun, Leisenring, Jarron M., Lin, Yen-Ting, Liu, Jian, Long, Daniel C., Loomis, Craig P., Lucatello, Sara, Lundgren, Britt, Lupton, Robert H., Ma, Bo, Ma, Zhibo, MacDonald, Nicholas, Mack, Claude, Mahadevan, Suvrath, Maia, Marcio A. G., Majewski, Steven R., Makler, Martin, Malanushenko, Elena, Malanushenko, Viktor, Mandelbaum, Rachel, Maraston, Claudia, Margala, Daniel, Maseman, Paul, Masters, Karen L., McBride, Cameron K., McDonald, Patrick, McGreer, Ian D., McMahon, Richard G., Mena Requejo, Olga, Ménard, Brice, Miralda-Escudé, Jordi, Morrison, Heather L., Mullally, Fergal, Muna, Demitri, Murayama, Hitoshi, Myers, Adam D., Naugle, Tracy, Neto, Angelo Fausti, Nguyen, Duy Cuong, Nichol, Robert C., Nidever, David L., O’Connell, Robert W., Ogando, Ricardo L. C., Olmstead, Matthew D., Oravetz, Daniel J., Padmanabhan, Nikhil, Paegert, Martin, Palanque-Delabrouille, Nathalie, Pan, Kaike, Pandey, Parul, Parejko, John K., Pâris, Isabelle, Pellegrini, Paulo, Pepper, Joshua, Percival, Will J., Petitjean, Patrick, Pfaffenberger, Robert, Pforr, Janine, Phleps, Stefanie, Pichon, Christophe, Pieri, Matthew M., Prada, Francisco, Price-Whelan, Adrian M., Raddick, M. Jordan, Ramos, Beatriz H. F., Reid, I. Neill, Reyle, Celine, Rich, James, Richards, Gordon T., Rieke, George H., Rieke, Marcia J., Rix, Hans-Walter, Robin, Annie C., Rocha-Pinto, Helio J., Rockosi, Constance M., Roe, Natalie A., Rollinde, Emmanuel, Ross, Ashley J., Ross, Nicholas P., Rossetto, Bruno, Sánchez, Ariel G., Santiago, Basilio, Sayres, Conor, Schiavon, Ricardo, Schlegel, David J., Schlesinger, Katharine J., Schmidt, Sarah J., Schneider, Donald P., Sellgren, Kris, Shelden, Alaina, Sheldon, Erin, Shetrone, Matthew, Shu, Yiping, Silverman, John D., Simmerer, Jennifer, Simmons, Audrey E., Sivarani, Thirupathi, Skrutskie, M. F., Slosar, Anže, Smee, Stephen, Smith, Verne V., Snedden, Stephanie A., Stassun, Keivan G., Steele, Oliver, Steinmetz, Matthias, Stockett, Mark H., Stollberg, Todd, Strauss, Michael A., Szalay, Alexander S., Tanaka, Masayuki, Thakar, Aniruddha R., Thomas, Daniel, Tinker, Jeremy L., Tofflemire, Benjamin M., Tojeiro, Rita, Tremonti, Christy A., Vargas Magaña, Mariana, Verde, Licia, Vogt, Nicole P., Wake, David A., Wan, Xiaoke, Wang, Ji, Weaver, Benjamin A., White, Martin, White, Simon D. M., Wilson, John C., Wisniewski, John P., Wood-Vasey, W. Michael, Yanny, Brian, Yasuda, Naoki, Yèche, Christophe, York, Donald G., Young, Erick, Zasowski, Gail, Zehavi, Idit, Zhao, Bo, Eisenstein, Daniel J., Weinberg, David H., Agol, Eric, Aihara, Hiroaki, Allende Prieto, Carlos, Anderson, Scott F., Arns, James A., Aubourg, Éric, Bailey, Stephen, Balbinot, Eduardo, Barkhouser, Robert, Beers, Timothy C., Berlind, Andreas A., Bickerton, Steven J., Bizyaev, Dmitry, Blanton, Michael R., Bochanski, John J., Bolton, Adam S., Bosman, Casey T., Bovy, Jo, Brandt, W. N., Breslauer, Ben, Brewington, Howard J., Brinkmann, J., Brown, Peter J., Brownstein, Joel R., Burger, Dan, Busca, Nicolas G., Campbell, Heather, Cargile, Phillip A., Carithers, William C., Carlberg, Joleen K., Carr, Michael A., Chang, Liang, Chen, Yanmei, Chiappini, Cristina, Comparat, Johan, Connolly, Natalia, Cortes, Marina, Croft, Rupert A. C., Cunha, Katia, da Costa, Luiz N., Davenport, James R. 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F., Slosar, Anže, Smee, Stephen, Smith, Verne V., Snedden, Stephanie A., Stassun, Keivan G., Steele, Oliver, Steinmetz, Matthias, Stockett, Mark H., Stollberg, Todd, Strauss, Michael A., Szalay, Alexander S., Tanaka, Masayuki, Thakar, Aniruddha R., Thomas, Daniel, Tinker, Jeremy L., Tofflemire, Benjamin M., Tojeiro, Rita, Tremonti, Christy A., Vargas Magaña, Mariana, Verde, Licia, Vogt, Nicole P., Wake, David A., Wan, Xiaoke, Wang, Ji, Weaver, Benjamin A., White, Martin, White, Simon D. M., Wilson, John C., Wisniewski, John P., Wood-Vasey, W. Michael, Yanny, Brian, Yasuda, Naoki, Yèche, Christophe, York, Donald G., Young, Erick, Zasowski, Gail, Zehavi, Idit, and Zhao, Bo

Abstract

Building on the legacy of the Sloan Digital Sky Survey (SDSS-I and II), SDSS-III is a program of four spectroscopic surveys on three scientific themes: dark energy and cosmological parameters, the history and structure of the Milky Way, and the population of giant planets around other stars. In keeping with SDSS tradition, SDSS-III will provide regular public releases of all its data, beginning with SDSS Data Release 8 (DR8), which was made public in 2011 January and includes SDSS-I and SDSS-II images and spectra reprocessed with the latest pipelines and calibrations produced for the SDSS-III investigations. This paper presents an overview of the four surveys that comprise SDSS-III. The Baryon Oscillation Spectroscopic Survey will measure redshifts of 1.5 million massive galaxies and Lyα forest spectra of 150,000 quasars, using the baryon acoustic oscillation feature of large-scale structure to obtain percent-level determinations of the distance scale and Hubble expansion rate at z < 0.7 and at z ≈ 2.5. SEGUE-2, an already completed SDSS-III survey that is the continuation of the SDSS-II Sloan Extension for Galactic Understanding and Exploration (SEGUE), measured medium-resolution (R = λ/Δλ ≈ 1800) optical spectra of 118,000 stars in a variety of target categories, probing chemical evolution, stellar kinematics and substructure, and the mass profile of the dark matter halo from the solar neighborhood to distances of 100 kpc. APOGEE, the Apache Point Observatory Galactic Evolution Experiment, will obtain high-resolution (R ≈ 30,000), high signal-to-noise ratio (S/N ≥ 100 per resolution element), H-band (1.51μm < λ < 1.70μm) spectra of 105 evolved, late-type stars, measuring separate abundances for ~15 elements per star and creating the first high-precision spectroscopic survey of all Galactic stellar populations (bulge, bar, disks, halo) with a uniform set of stellar tracers and spectral diagnostics. The Multi-object APO Radial Velocity Exoplanet La

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