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101. A Large Catalog of Accurate Distances to Molecular Clouds from PS1 Photometry

Author: Schlafly, E. F., Green, G., Finkbeiner, D. P., Rix, H. -W., Bell, E. F., Burgett, W. S., Chambers, K. C., Draper, P. W., Hodapp, K. W., Kaiser, N., Magnier, E. A., Martin, N. F., Metcalfe, N., Price, P. A., and Tonry, J. L.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Distance measurements to molecular clouds are important, but are often made separately for each cloud of interest, employing very different different data and techniques. We present a large, homogeneous catalog of distances to molecular clouds, most of which are of unprecedented accuracy. We determine distances using optical photometry of stars along lines of sight toward these clouds, obtained from PanSTARRS-1. We simultaneously infer the reddenings and distances to these stars, tracking the full probability distribution function using a technique presented in Green et al. (2014). We fit these star-by-star measurements using a simple dust screen model to find the distance to each cloud. We thus estimate the distances to almost all of the clouds in the Magnani et al. (1985) catalog, as well as many other well-studied clouds, including Orion, Perseus, Taurus, Cepheus, Polaris, California, and Monoceros R2, avoiding only the inner Galaxy. Typical statistical uncertainties in the distances are 5%, though the systematic uncertainty stemming from the quality of our stellar models is about 10%. The resulting catalog is the largest catalog of accurate, directly-measured distances to molecular clouds. Our distance estimates are generally consistent with available distance estimates from the literature, though in some cases the literature estimates are off by a factor of more than two., Comment: 16 pages, 4 figures
Published: 2014
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102. Discovery of a dormant 33 solar-mass black hole in pre-release Gaia astrometry

Author: Panuzzo, P., Mazeh, T., Arenou, F., Holl, B., Caffau, E., Jorissen, A., Babusiaux, C., Gavras, P., Sahlmann, J., Bastian, U., Wyrzykowski, Ł., Eyer, L., Leclerc, N., Bauchet, N., Bombrun, A., Mowlavi, N., Seabroke, G. M., Teyssier, D., Balbinot, E., Helmi, A., Brown, A. G.A., Vallenari, A., Prusti, T., De Bruijne, J. H.J., Barbier, A., Biermann, M., Creevey, O. L., Ducourant, C., Evans, D. W., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Nicolas, C., Randich, S., Sartoretti, P., Smiljanic, R., Tanga, P., Walton, N. A., Aerts, C., Bailer-Jones, C. A.L., Cropper, M., Drimmel, R., Jansen, F., Katz, D., Lattanzi, M. G., Soubiran, C., Thévenin, F., Van Leeuwen, F., Andrae, R., Audard, M., Bakker, J., Blomme, R., Castañeda, J., De Angeli, F., Fabricius, C., Fouesneau, M., Frémat, Y., Galluccio, L., Guerrier, A., Heiter, U., Masana, E., Messineo, R., Nienartowicz, K., Pailler, F., Riclet, F., Roux, W., Sordo, R., Gracia-Abril, G., Portell, J., Altmann, M., Benson, K., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Cacciari, C., Cánovas, H., Carrasco, J. M., Carry, B., Cellino, A., Cheek, N., Clementini, G., Damerdji, Y., Davidson, M., De Teodoro, P., Delchambre, L., Della Oro, A., Fraile Garcia, E., Garabato, D., García-Lario, P., Haigron, R., Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hernández, J., Hestroffer, D., Hodgkin, S. T., Jamal, S., Jevardat De Fombelle, G., Jordan, S., Krone-Martins, A., Lanzafame, A. C., Löffler, W., Lorca, A., Marchal, O., Marrese, P. M., Moitinho, A., Muinonen, K., Nuñez Campos, M., Oreshina-Slezak, I., Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Rimoldini, L., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Smith, M., Sozzetti, A., Utrilla, E., Van Leeuwen, M., Weingrill, K., Abbas, U., Ábrahám, P., Abreu Aramburu, A., Ahmed, S., Altavilla, G., Álvarez, M. A., Anders, F., Anderson, R. I., Anglada Varela, E., Antoja, T., Baig, S., Baines, D., Baker, S. G., Balaguer-Núñez, L., Balog, Z., Barache, C., Barros, M., Barstow, M. A., Bartolomé, S., Bashi, D., Bassilana, J. L., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Blanco-Cuaresma, S., Bland-Hawthorn, J., Blazere, A., Boch, T., Bossini, D., Bouquillon, S., Bragaglia, A., Braine, J., Bratsolis, E., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Camut, A., Cancelliere, R., Cantat-Gaudin, T., Capilla Guilarte, D., Carballo, R., Carlucci, T., Carnerero, M. I., Carretero, J., Carton, S., Casamiquela, L., Casey, A., Castellani, M., Castro-Ginard, A., Ceraj, L., Cesare, V., Charlot, P., Chaudet, C., Chemin, L., Chiavassa, A., Chornay, N., Chosson, D., Cooper, W. J., Cornez, T., Cowell, S., Crosta, M., Crowley, C., Cruz Reyes, M., Dafonte, C., Dal Ponte, M., David, M., De Laverny, P., De Luise, F., De March, R., De Torres, A., Del Peloso, E. F., Delbo, M., Delgado, A., Delisle, J. B., Demouchy, C., Denis, E., Dharmawardena, T. E., Di Giacomo, F., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Enke, H., Fabre, C., Fabrizio, M., Faigler, S., Fatoviä, M., Fedorets, G., Fernández-Hernández, J., Fernique, P., Figueras, F., Fouron, C., Fragkoudi, F., Gai, M., Galinier, M., Garcia-Serrano, A., García-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomboc, A., Gomez, A., González-Santamaría, I., Gosset, E., Granvik, Mikael, Gregori Barrera, V., Gutiérrez-Sánchez, R., Haywood, M., Helmer, A., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., Jiménez-Arranz, Ó., Juaristi Campillo, J., Kaczmarek, Z., Kervella, P., Khanna, S., Kontizas, M., Kordopatis, G., Korn, A. J., Kóspál, Á., Kostrzewa-Rutkowska, Z., KruszyåÃ Â Ska, K., Kun, M., Lambert, S., Lanza, A. F., Lebreton, Y., Lebzelter, T., Leccia, S., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Livanou, E., Lobel, A., López-Miralles, J., Loup, C., Madarász, M., Mahy, L., Mann, R. G., Manteiga, M., Marcellino, C. P., Marchant, J. M., Marconi, M., Marín Pina, D., Marinoni, S., Marshall, D. J., Martín Lozano, J., Martin Polo, L., Martín-Fleitas, J. M., Marton, G., Mascarenhas, D., Masip, A., Mastrobuono-Battisti, A., McMillan, P. J., Meichsner, J., Merc, J., Messina, S., Millar, N. R., Mints, A., Mohamed, D., Molina, D., Molinaro, R., Molnár, L., Monguió, M., Montegriffo, P., Monti, L., Mora, A., Morbidelli, R., Morris, D., Mudimadugula, R., Muraveva, T., Musella, I., Nagy, Z., Nardetto, N., Navarrete, C., Oh, S., Ordenovic, C., Orenstein, O., Pagani, C., Pagano, I., Palaversa, L., Palicio, P. A., Pallas-Quintela, L., Pawlak, M., Penttilä, A., Pesciullesi, P., Pinamonti, M., Plachy, E., Planquart, L., Plum, G., Poggio, E., Pourbaix, D., Price-Whelan, A. M., Pulone, L., Rabin, V., Rainer, M., Raiteri, C. M., Ramos, P., Ramos-Lerate, M., Ratajczak, M., Re Fiorentin, P., Regibo, S., Reylé, C., Ripepi, V., Riva, A., Rix, H. W., Rixon, G., Robert, G., Robichon, N., Robin, C., Romero-Gómez, M., Rowell, N., Ruz Mieres, D., Rybicki, K. A., Sadowski, G., Sagristà Sellés, A., Sanna, N., Santoveña, R., Sarasso, M., Sarmiento, M. H., Sarrate Riera, C., Sciacca, E., Ségransan, D., Semczuk, M., Shahaf, S., Siebert, A., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmüller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., Teixeira, R., Tepper-Garcia, T., Thuillot, W., Tolomei, L., Tonello, N., Torra, F., Torralba Elipe, G., Trabucchi, M., Trentin, E., Tsantaki, M., Turon, C., Ulla, A., Unger, N., Valtchanov, I., Vanel, O., Vecchiato, A., Vicente, D., Villar, E., Weiler, M., Zhao, H., Zorec, J., Zucker, S., Župiä, A., Zwitter, T., Panuzzo, P., Mazeh, T., Arenou, F., Holl, B., Caffau, E., Jorissen, A., Babusiaux, C., Gavras, P., Sahlmann, J., Bastian, U., Wyrzykowski, Ł., Eyer, L., Leclerc, N., Bauchet, N., Bombrun, A., Mowlavi, N., Seabroke, G. M., Teyssier, D., Balbinot, E., Helmi, A., Brown, A. G.A., Vallenari, A., Prusti, T., De Bruijne, J. H.J., Barbier, A., Biermann, M., Creevey, O. L., Ducourant, C., Evans, D. W., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Nicolas, C., Randich, S., Sartoretti, P., Smiljanic, R., Tanga, P., Walton, N. A., Aerts, C., Bailer-Jones, C. A.L., Cropper, M., Drimmel, R., Jansen, F., Katz, D., Lattanzi, M. G., Soubiran, C., Thévenin, F., Van Leeuwen, F., Andrae, R., Audard, M., Bakker, J., Blomme, R., Castañeda, J., De Angeli, F., Fabricius, C., Fouesneau, M., Frémat, Y., Galluccio, L., Guerrier, A., Heiter, U., Masana, E., Messineo, R., Nienartowicz, K., Pailler, F., Riclet, F., Roux, W., Sordo, R., Gracia-Abril, G., Portell, J., Altmann, M., Benson, K., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Cacciari, C., Cánovas, H., Carrasco, J. M., Carry, B., Cellino, A., Cheek, N., Clementini, G., Damerdji, Y., Davidson, M., De Teodoro, P., Delchambre, L., Della Oro, A., Fraile Garcia, E., Garabato, D., García-Lario, P., Haigron, R., Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hernández, J., Hestroffer, D., Hodgkin, S. T., Jamal, S., Jevardat De Fombelle, G., Jordan, S., Krone-Martins, A., Lanzafame, A. C., Löffler, W., Lorca, A., Marchal, O., Marrese, P. M., Moitinho, A., Muinonen, K., Nuñez Campos, M., Oreshina-Slezak, I., Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Rimoldini, L., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Smith, M., Sozzetti, A., Utrilla, E., Van Leeuwen, M., Weingrill, K., Abbas, U., Ábrahám, P., Abreu Aramburu, A., Ahmed, S., Altavilla, G., Álvarez, M. A., Anders, F., Anderson, R. I., Anglada Varela, E., Antoja, T., Baig, S., Baines, D., Baker, S. G., Balaguer-Núñez, L., Balog, Z., Barache, C., Barros, M., Barstow, M. A., Bartolomé, S., Bashi, D., Bassilana, J. L., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Blanco-Cuaresma, S., Bland-Hawthorn, J., Blazere, A., Boch, T., Bossini, D., Bouquillon, S., Bragaglia, A., Braine, J., Bratsolis, E., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Camut, A., Cancelliere, R., Cantat-Gaudin, T., Capilla Guilarte, D., Carballo, R., Carlucci, T., Carnerero, M. I., Carretero, J., Carton, S., Casamiquela, L., Casey, A., Castellani, M., Castro-Ginard, A., Ceraj, L., Cesare, V., Charlot, P., Chaudet, C., Chemin, L., Chiavassa, A., Chornay, N., Chosson, D., Cooper, W. J., Cornez, T., Cowell, S., Crosta, M., Crowley, C., Cruz Reyes, M., Dafonte, C., Dal Ponte, M., David, M., De Laverny, P., De Luise, F., De March, R., De Torres, A., Del Peloso, E. F., Delbo, M., Delgado, A., Delisle, J. B., Demouchy, C., Denis, E., Dharmawardena, T. E., Di Giacomo, F., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Enke, H., Fabre, C., Fabrizio, M., Faigler, S., Fatoviä, M., Fedorets, G., Fernández-Hernández, J., Fernique, P., Figueras, F., Fouron, C., Fragkoudi, F., Gai, M., Galinier, M., Garcia-Serrano, A., García-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomboc, A., Gomez, A., González-Santamaría, I., Gosset, E., Granvik, Mikael, Gregori Barrera, V., Gutiérrez-Sánchez, R., Haywood, M., Helmer, A., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., Jiménez-Arranz, Ó., Juaristi Campillo, J., Kaczmarek, Z., Kervella, P., Khanna, S., Kontizas, M., Kordopatis, G., Korn, A. J., Kóspál, Á., Kostrzewa-Rutkowska, Z., KruszyåÃ Â Ska, K., Kun, M., Lambert, S., Lanza, A. F., Lebreton, Y., Lebzelter, T., Leccia, S., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Livanou, E., Lobel, A., López-Miralles, J., Loup, C., Madarász, M., Mahy, L., Mann, R. G., Manteiga, M., Marcellino, C. P., Marchant, J. M., Marconi, M., Marín Pina, D., Marinoni, S., Marshall, D. J., Martín Lozano, J., Martin Polo, L., Martín-Fleitas, J. M., Marton, G., Mascarenhas, D., Masip, A., Mastrobuono-Battisti, A., McMillan, P. J., Meichsner, J., Merc, J., Messina, S., Millar, N. R., Mints, A., Mohamed, D., Molina, D., Molinaro, R., Molnár, L., Monguió, M., Montegriffo, P., Monti, L., Mora, A., Morbidelli, R., Morris, D., Mudimadugula, R., Muraveva, T., Musella, I., Nagy, Z., Nardetto, N., Navarrete, C., Oh, S., Ordenovic, C., Orenstein, O., Pagani, C., Pagano, I., Palaversa, L., Palicio, P. A., Pallas-Quintela, L., Pawlak, M., Penttilä, A., Pesciullesi, P., Pinamonti, M., Plachy, E., Planquart, L., Plum, G., Poggio, E., Pourbaix, D., Price-Whelan, A. M., Pulone, L., Rabin, V., Rainer, M., Raiteri, C. M., Ramos, P., Ramos-Lerate, M., Ratajczak, M., Re Fiorentin, P., Regibo, S., Reylé, C., Ripepi, V., Riva, A., Rix, H. W., Rixon, G., Robert, G., Robichon, N., Robin, C., Romero-Gómez, M., Rowell, N., Ruz Mieres, D., Rybicki, K. A., Sadowski, G., Sagristà Sellés, A., Sanna, N., Santoveña, R., Sarasso, M., Sarmiento, M. H., Sarrate Riera, C., Sciacca, E., Ségransan, D., Semczuk, M., Shahaf, S., Siebert, A., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmüller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., Teixeira, R., Tepper-Garcia, T., Thuillot, W., Tolomei, L., Tonello, N., Torra, F., Torralba Elipe, G., Trabucchi, M., Trentin, E., Tsantaki, M., Turon, C., Ulla, A., Unger, N., Valtchanov, I., Vanel, O., Vecchiato, A., Vicente, D., Villar, E., Weiler, M., Zhao, H., Zorec, J., Zucker, S., Župiä, A., and Zwitter, T.
Abstract: Context. Gravitational waves from black-hole (BH) merging events have revealed a population of extra-galactic BHs residing in short-period binaries with masses that are higher than expected based on most stellar evolution models-And also higher than known stellar-origin black holes in our Galaxy. It has been proposed that those high-mass BHs are the remnants of massive metal-poor stars. Aims. Gaia astrometry is expected to uncover many Galactic wide-binary systems containing dormant BHs, which may not have been detected before. The study of this population will provide new information on the BH-mass distribution in binaries and shed light on their formation mechanisms and progenitors. Methods. As part of the validation efforts in preparation for the fourth Gaia data release (DR4), we analysed the preliminary astrometric binary solutions, obtained by the Gaia Non-Single Star pipeline, to verify their significance and to minimise false-detection rates in high-mass-function orbital solutions. Results. The astrometric binary solution of one source, Gaia BH3, implies the presence of a 32.70a ±a 0.82aM- BH in a binary system with a period of 11.6 yr. Gaia radial velocities independently validate the astrometric orbit. Broad-band photometric and spectroscopic data show that the visible component is an old, very metal-poor giant of the Galactic halo, at a distance of 590 pc. Conclusions. The BH in the Gaia BH3 system is more massive than any other Galactic stellar-origin BH known thus far. The low metallicity of the star companion supports the scenario that metal-poor massive stars are progenitors of the high-mass BHs detected by gravitational-wave telescopes. The Galactic orbit of the system and its metallicity indicate that it might belong to the Sequoia halo substructure. Alternatively, and more plausibly, it could belong to the ED-2 stream, which likely originated from a globular cluster that had been disrupted by the Milky Way., Funder: for funder information see Appendix F in https://doi.org/10.1051/0004-6361/202449763;Full text license: CC BY 4.0
Published: 2024
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103. Gaia Focused Product Release: A catalogue of sources around quasars to search for strongly lensed quasars

Author: Krone-Martins, A., Ducourant, C., Galluccio, L., Delchambre, L., Oreshina-Slezak, I., Teixeira, R., Braine, J., Le Campion, J. F., Mignard, F., Roux, W., Blazere, A., Pegoraro, L., Brown, A. G.A., Vallenari, A., Prusti, T., De Bruijne, J. H.J., Arenou, F., Babusiaux, C., Barbier, A., Biermann, M., Creevey, O. L., Evans, D. W., Eyer, L., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Randich, S., Sartoretti, P., Smiljanic, R., Tanga, P., Walton, N. A., Bailer-Jones, C. A.L., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Soubiran, C., Van Leeuwen, F., Audard, M., Bakker, J., Blomme, R., Castañeda, J., De Angeli, F., Fabricius, C., Fouesneau, M., Frémat, Y., Guerrier, A., Masana, E., Messineo, R., Nicolas, C., Nienartowicz, K., Pailler, F., Panuzzo, P., Riclet, F., Seabroke, G. M., Sordo, R., Thévenin, F., Gracia-Abril, G., Portell, J., Teyssier, D., Altmann, M., Benson, K., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Cánovas, H., Carry, B., Cheek, N., Clementini, G., Damerdji, Y., Davidson, M., De Teodoro, P., Dell' Oro, A., Fraile Garcia, E., Garabato, D., García-Lario, P., Garralda Torres, N., Gavras, P., Haigron, R., Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hernández, J., Hodgkin, S. T., Holl, B., Jamal, S., Jordan, S., Lanzafame, A. C., Löffler, W., Lorca, A., Marchal, O., Marrese, P. M., Moitinho, A., Muinonen, K., Nuñez Campos, M., Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Rimoldini, L., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Siopis, C., Smith, M., Sozzetti, A., Utrilla, E., Van Leeuwen, M., Weingrill, K., Abbas, U., Ábrahám, P., Abreu Aramburu, A., Aerts, C., Altavilla, G., Álvarez, M. A., Alves, J., Anderson, R. I., Antoja, T., Baines, D., Baker, S. G., Balog, Z., Barache, C., Barbato, D., Barros, M., Barstow, M. A., Bartolomé, S., Bashi, D., Bauchet, N., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Berihuete, A., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Boch, T., Bombrun, A., Bouquillon, S., Bragaglia, A., Bramante, L., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzo, S., Carballo, R., Carlucci, T., Carnerero, M. I., Carrasco, J. M., Carretero, J., Carton, S., Casamiquela, L., Castellani, M., Castro-Ginard, A., Cesare, V., Charlot, P., Chemin, L., Chiaramida, V., Chiavassa, A., Chornay, N., Collins, R., Contursi, G., Cooper, W. J., Cornez, T., Crosta, M., Crowley, C., Dafonte, C., De Laverny, P., De Luise, F., De March, R., De Souza, R., De Torres, A., Del Peloso, E. F., Delbo, M., Delgado, A., Dharmawardena, T. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Durán, J., Enke, H., Esquej, P., Fabre, C., Fabrizio, M., Faigler, S., FatoviäÃ Â‡, M., Fedorets, G., Fernández-Hernández, J., Fernique, P., Figueras, F., Fournier, Y., Fouron, C., Gai, M., Galinier, M., Garcia-Gutierrez, A., García-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomel, R., Gomez, A., González-Núñez, J., González-Santamaría, I., Gosset, E., Granvik, Mikael, Gregori Barrera, V., Gutiérrez-Sánchez, R., Haywood, M., Helmer, A., Helmi, A., Henares, K., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., JabåÃ Â OåÃ Â., Ska, M., Jansen, F., Jiménez-Arranz, Ó, Juaristi Campillo, J., Khanna, S., Kordopatis, G., Kóspál, Á, Kostrzewa-Rutkowska, Z., Kun, M., Lambert, S., Lanza, A. F., Lebreton, Y., Lebzelter, T., Leccia, S., Lecoeur-Taibi, I., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Lindstrøm, H. E.P., Lister, T. A., Livanou, E., Lobel, A., Loup, C., Mahy, L., Mann, R. G., Manteiga, M., Marchant, J. M., Marconi, M., Marín Pina, D., Marinoni, S., Marshall, D. J., Martín Lozano, J., Martín-Fleitas, J. M., Marton, G., Mary, N., Masip, A., Massari, D., Mastrobuono-Battisti, A., Mazeh, T., McMillan, P. J., Meichsner, J., Messina, S., Michalik, D., Millar, N. R., Mints, A., Molina, D., Molinaro, R., Molnár, L., Monari, G., Monguió, M., Montegriffo, P., Montero, A., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morris, D., Mowlavi, N., Munoz, D., Muraveva, T., Murphy, C. P., Musella, I., Nagy, Z., Nieto, S., Noval, L., Ogden, A., Ordenovic, C., Pagani, C., Pagano, I., Palaversa, L., Palicio, P. A., Pallas-Quintela, L., Panahi, A., Panem, C., Payne-Wardenaar, S., Penttilä, A., Pesciullesi, P., Piersimoni, A. M., Pinamonti, M., Pineau, F. X., Plachy, E., Plum, G., Poggio, E., Pourbaix, D., Prša, A., Pulone, L., Racero, E., Rainer, M., Raiteri, C. M., Ramos, P., Ramos-Lerate, M., Ratajczak, M., Re Fiorentin, P., Regibo, S., Reylé, C., Ripepi, V., Riva, A., Rix, H. W., Rixon, G., Robichon, N., Robin, C., Romero-Gómez, M., Rowell, N., Royer, F., Ruz Mieres, D., Rybicki, K. A., Sadowski, G., Sáez Núñez, A., Sagristà Sellés, A., Sahlmann, J., Sanchez Gimenez, V., Sanna, N., Santoveña, R., Sarasso, M., Sarrate Riera, C., Sciacca, E., Segovia, J. C., Ségransan, D., Shahaf, S., Siebert, A., Siltala, L., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spina, L., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmüller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., TisaniäÃ Â‡, K., Tolomei, L., Torra, F., Torralba Elipe, G., Trabucchi, M., Tsantaki, M., Ulla, A., Unger, N., Vanel, O., Vecchiato, A., Vicente, D., Voutsinas, S., Weiler, M., Wyrzykowski, Ł, Zhao, H., Zorec, J., Zwitter, T., Balaguer-Núñez, L., Leclerc, N., Morgenthaler, S., Robert, G., Zucker, S., Krone-Martins, A., Ducourant, C., Galluccio, L., Delchambre, L., Oreshina-Slezak, I., Teixeira, R., Braine, J., Le Campion, J. F., Mignard, F., Roux, W., Blazere, A., Pegoraro, L., Brown, A. G.A., Vallenari, A., Prusti, T., De Bruijne, J. H.J., Arenou, F., Babusiaux, C., Barbier, A., Biermann, M., Creevey, O. L., Evans, D. W., Eyer, L., Guerra, R., Hutton, A., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Randich, S., Sartoretti, P., Smiljanic, R., Tanga, P., Walton, N. A., Bailer-Jones, C. A.L., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Soubiran, C., Van Leeuwen, F., Audard, M., Bakker, J., Blomme, R., Castañeda, J., De Angeli, F., Fabricius, C., Fouesneau, M., Frémat, Y., Guerrier, A., Masana, E., Messineo, R., Nicolas, C., Nienartowicz, K., Pailler, F., Panuzzo, P., Riclet, F., Seabroke, G. M., Sordo, R., Thévenin, F., Gracia-Abril, G., Portell, J., Teyssier, D., Altmann, M., Benson, K., Berthier, J., Burgess, P. W., Busonero, D., Busso, G., Cánovas, H., Carry, B., Cheek, N., Clementini, G., Damerdji, Y., Davidson, M., De Teodoro, P., Dell' Oro, A., Fraile Garcia, E., Garabato, D., García-Lario, P., Garralda Torres, N., Gavras, P., Haigron, R., Hambly, N. C., Harrison, D. L., Hatzidimitriou, D., Hernández, J., Hodgkin, S. T., Holl, B., Jamal, S., Jordan, S., Lanzafame, A. C., Löffler, W., Lorca, A., Marchal, O., Marrese, P. M., Moitinho, A., Muinonen, K., Nuñez Campos, M., Osborne, P., Pancino, E., Pauwels, T., Recio-Blanco, A., Riello, M., Rimoldini, L., Robin, A. C., Roegiers, T., Sarro, L. M., Schultheis, M., Siopis, C., Smith, M., Sozzetti, A., Utrilla, E., Van Leeuwen, M., Weingrill, K., Abbas, U., Ábrahám, P., Abreu Aramburu, A., Aerts, C., Altavilla, G., Álvarez, M. A., Alves, J., Anderson, R. I., Antoja, T., Baines, D., Baker, S. G., Balog, Z., Barache, C., Barbato, D., Barros, M., Barstow, M. A., Bartolomé, S., Bashi, D., Bauchet, N., Baudeau, N., Becciani, U., Bedin, L. R., Bellas-Velidis, I., Bellazzini, M., Beordo, W., Berihuete, A., Bernet, M., Bertolotto, C., Bertone, S., Bianchi, L., Binnenfeld, A., Boch, T., Bombrun, A., Bouquillon, S., Bragaglia, A., Bramante, L., Breedt, E., Bressan, A., Brouillet, N., Brugaletta, E., Bucciarelli, B., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzo, S., Carballo, R., Carlucci, T., Carnerero, M. I., Carrasco, J. M., Carretero, J., Carton, S., Casamiquela, L., Castellani, M., Castro-Ginard, A., Cesare, V., Charlot, P., Chemin, L., Chiaramida, V., Chiavassa, A., Chornay, N., Collins, R., Contursi, G., Cooper, W. J., Cornez, T., Crosta, M., Crowley, C., Dafonte, C., De Laverny, P., De Luise, F., De March, R., De Souza, R., De Torres, A., Del Peloso, E. F., Delbo, M., Delgado, A., Dharmawardena, T. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Dsilva, K., Durán, J., Enke, H., Esquej, P., Fabre, C., Fabrizio, M., Faigler, S., FatoviäÃ Â‡, M., Fedorets, G., Fernández-Hernández, J., Fernique, P., Figueras, F., Fournier, Y., Fouron, C., Gai, M., Galinier, M., Garcia-Gutierrez, A., García-Torres, M., Garofalo, A., Gerlach, E., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Gomel, R., Gomez, A., González-Núñez, J., González-Santamaría, I., Gosset, E., Granvik, Mikael, Gregori Barrera, V., Gutiérrez-Sánchez, R., Haywood, M., Helmer, A., Helmi, A., Henares, K., Hidalgo, S. L., Hilger, T., Hobbs, D., Hottier, C., Huckle, H. E., JabåÃ Â OåÃ Â., Ska, M., Jansen, F., Jiménez-Arranz, Ó, Juaristi Campillo, J., Khanna, S., Kordopatis, G., Kóspál, Á, Kostrzewa-Rutkowska, Z., Kun, M., Lambert, S., Lanza, A. F., Lebreton, Y., Lebzelter, T., Leccia, S., Lecoeur-Taibi, I., Lecoutre, G., Liao, S., Liberato, L., Licata, E., Lindstrøm, H. E.P., Lister, T. A., Livanou, E., Lobel, A., Loup, C., Mahy, L., Mann, R. G., Manteiga, M., Marchant, J. M., Marconi, M., Marín Pina, D., Marinoni, S., Marshall, D. J., Martín Lozano, J., Martín-Fleitas, J. M., Marton, G., Mary, N., Masip, A., Massari, D., Mastrobuono-Battisti, A., Mazeh, T., McMillan, P. J., Meichsner, J., Messina, S., Michalik, D., Millar, N. R., Mints, A., Molina, D., Molinaro, R., Molnár, L., Monari, G., Monguió, M., Montegriffo, P., Montero, A., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morris, D., Mowlavi, N., Munoz, D., Muraveva, T., Murphy, C. P., Musella, I., Nagy, Z., Nieto, S., Noval, L., Ogden, A., Ordenovic, C., Pagani, C., Pagano, I., Palaversa, L., Palicio, P. A., Pallas-Quintela, L., Panahi, A., Panem, C., Payne-Wardenaar, S., Penttilä, A., Pesciullesi, P., Piersimoni, A. M., Pinamonti, M., Pineau, F. X., Plachy, E., Plum, G., Poggio, E., Pourbaix, D., Prša, A., Pulone, L., Racero, E., Rainer, M., Raiteri, C. M., Ramos, P., Ramos-Lerate, M., Ratajczak, M., Re Fiorentin, P., Regibo, S., Reylé, C., Ripepi, V., Riva, A., Rix, H. W., Rixon, G., Robichon, N., Robin, C., Romero-Gómez, M., Rowell, N., Royer, F., Ruz Mieres, D., Rybicki, K. A., Sadowski, G., Sáez Núñez, A., Sagristà Sellés, A., Sahlmann, J., Sanchez Gimenez, V., Sanna, N., Santoveña, R., Sarasso, M., Sarrate Riera, C., Sciacca, E., Segovia, J. C., Ségransan, D., Shahaf, S., Siebert, A., Siltala, L., Slezak, E., Smart, R. L., Snaith, O. N., Solano, E., Solitro, F., Souami, D., Souchay, J., Spina, L., Spitoni, E., Spoto, F., Squillante, L. A., Steele, I. A., Steidelmüller, H., Surdej, J., Szabados, L., Taris, F., Taylor, M. B., TisaniäÃ Â‡, K., Tolomei, L., Torra, F., Torralba Elipe, G., Trabucchi, M., Tsantaki, M., Ulla, A., Unger, N., Vanel, O., Vecchiato, A., Vicente, D., Voutsinas, S., Weiler, M., Wyrzykowski, Ł, Zhao, H., Zorec, J., Zwitter, T., Balaguer-Núñez, L., Leclerc, N., Morgenthaler, S., Robert, G., and Zucker, S.
Abstract: Context. Strongly lensed quasars are fundamental sources for cosmology. The Gaia space mission covers the entire sky with the unprecedented resolution of 0.18âÃ Â€ ³ in the optical, making it an ideal instrument to search for gravitational lenses down to the limiting magnitude of 21. Nevertheless, the previous Gaia Data Releases are known to be incomplete for small angular separations such as those expected for most lenses. Aims. We present the Data Processing and Analysis Consortium GravLens pipeline, which was built to analyse all Gaia detections around quasars and to cluster them into sources, thus producing a catalogue of secondary sources around each quasar. We analysed the resulting catalogue to produce scores that indicate source configurations that are compatible with strongly lensed quasars. Methods. GravLens uses the DBSCAN unsupervised clustering algorithm to detect sources around quasars. The resulting catalogue of multiplets is then analysed with several methods to identify potential gravitational lenses. We developed and applied an outlier scoring method, a comparison between the average BP and RP spectra of the components, and we also used an extremely randomised tree algorithm. These methods produce scores to identify the most probable configurations and to establish a list of lens candidates. Results. We analysed the environment of 3 760 032 quasars. A total of 4 760 920 sources, including the quasars, were found within 6âÃ Â€ ³ of the quasar positions. This list is given in the Gaia archive. In 87% of cases, the quasar remains a single source, and in 501 385 cases neighbouring sources were detected. We propose a list of 381 lensed candidates, of which we identified 49 as the most promising ones. Beyond these candidates, the associate tables in this Focused Product Release allow the entire community to explore the unique Gaia data for strong lensing studies further., Full text license: CC BY 4.0;Funder: for funder information see Appendix C in https://doi.org/10.1051/0004-6361/202347273
Published: 2024
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104. Spectral Energy Distributions of QSOs at z>5: common AGN-heated dust and occasionally strong star-formation

Author: Leipski, C., Meisenheimer, K., Walter, F., Klaas, U., Dannerbauer, H., De Rosa, G., Fan, X., Haas, M., Krause, O., and Rix, H. -W.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present spectral energy distributions (SEDs) of 69 QSOs at z>5, covering a rest frame wavelength range of 0.1mu to ~80mu, and centered on new Spitzer and Herschel observations. The detection rate of the QSOs with Spitzer is very high (97% at lambda_rest ~< 4mu), but drops towards the Herschel bands with 30% detected in PACS (rest frame mid-infrared) and 15% additionally in the SPIRE (rest frame far-infrared; FIR). We perform multi-component SED fits for Herschel-detected objects and confirm that to match the observed SEDs, a clumpy torus model needs to be complemented by a hot (~1300K) component and, in cases with prominent FIR emission, also by a cold (~50K) component. In the FIR detected cases the luminosity of the cold component is on the order of 10^13 L_sun which is likely heated by star formation. From the SED fits we also determine that the AGN dust-to-accretion disk luminosity ratio declines with UV/optical luminosity. Emission from hot (~1300K) dust is common in our sample, showing that nuclear dust is ubiquitous in luminous QSOs out to redshift 6. However, about 15% of the objects appear under-luminous in the near infrared compared to their optical emission and seem to be deficient in (but not devoid of) hot dust. Within our full sample, the QSOs detected with Herschel are found at the high luminosity end in L_UV/opt and L_NIR and show low equivalent widths (EWs) in H_alpha and in Ly_alpha. In the distribution of H_alpha EWs, as determined from the Spitzer photometry, the high-redshift QSOs show little difference to low redshift AGN., Comment: 23 pages, 15 figures, 7 tables; accepted for publication in ApJ; a version of the paper including all online-only panels of Figure A.1 can be found at http://www.mpia-hd.mpg.de/homes/leipski/cleipski_2014_zgt5_sed_all.pdf
Published: 2014
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105. The Gaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

Author: Bergemann, M., Ruchti, G., Serenelli, A., Feltzing, S., Alves-Brito, A., Asplund, M., Bensby, T., Gruiters, P., Heiter, U., Korn, A., Lind, K., Marino, A., Jofre, P., Nordlander, T., Ryde, N., Gilmore, G., Randich, S., Ferguson, A., Jeffries, R., Micela, G., Negueruela, I., Prusti, T., Rix, H. -W., Vallenari, A., Alfaro, E. J., Prieto, C. Allende, Bragaglia, A., Koposov, S. E., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Walton, N., Costado, M. T., Franciosini, E., Hill, V., Lardo, C., de Laverny, P., Magrini, L., Maiorca, E., Masseron, T., Morbidelli, L., Sacco, G., Kordopatis, G., and Tautvaisiene, G.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We study the relationship between age, metallicity, and alpha-enhancement of FGK stars in the Galactic disk. The results are based upon the analysis of high-resolution UVES spectra from the Gaia-ESO large stellar survey. We explore the limitations of the observed dataset, i.e. the accuracy of stellar parameters and the selection effects that are caused by the photometric target preselection. We find that the colour and magnitude cuts in the survey suppress old metal-rich stars and young metal-poor stars. This suppression may be as high as 97% in some regions of the age-metallicity relationship. The dataset consists of 144 stars with a wide range of ages from 0.5 Gyr to 13.5 Gyr, Galactocentric distances from 6 kpc to 9.5 kpc, and vertical distances from the plane 0 < |Z| < 1.5 kpc. On this basis, we find that i) the observed age-metallicity relation is nearly flat in the range of ages between 0 Gyr and 8 Gyr; ii) at ages older than 9 Gyr, we see a decrease in [Fe/H] and a clear absence of metal-rich stars; this cannot be explained by the survey selection functions; iii) there is a significant scatter of [Fe/H] at any age; and iv) [Mg/Fe] increases with age, but the dispersion of [Mg/Fe] at ages > 9 Gyr is not as small as advocated by some other studies. In agreement with earlier work, we find that radial abundance gradients change as a function of vertical distance from the plane. The [Mg/Fe] gradient steepens and becomes negative. In addition, we show that the inner disk is not only more alpha-rich compared to the outer disk, but also older, as traced independently by the ages and Mg abundances of stars., Comment: accepted for publication in A&A
Published: 2014
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106. A Molecular Line Scan in the Hubble Deep Field North: Constraints on the CO Luminosity Function and the Cosmic H2 Density

Author: Walter, F., Decarli, R., Sargent, M., Carilli, C., Dickinson, M., Riechers, D., Ellis, R., Stark, D., Weiner, B., Aravena, M., Bell, E., Bertoldi, F., Cox, P., Da Cunha, E., Daddi, E., Downes, D., Lentati, L., Maiolino, R., Menten, K. M., Neri, R., Rix, H. W., and Weiss, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present direct constraints on the CO luminosity function at high redshift and the resulting cosmic evolution of the molecular gas density, $\rho_{\rm H2}$(z), based on a blind molecular line scan in the Hubble Deep Field North (HDF-N) using the IRAM Plateau de Bure Interferometer. Our line scan of the entire 3mm window (79-115 GHz) covers a cosmic volume of ~7000 Mpc$^3$, and redshift ranges z<0.45, 1.012. We use the rich multiwavelength and spectroscopic database of the HDF-N to derive some of the best constraints on CO luminosities in high redshift galaxies to date. We combine the blind CO detections in our molecular line scan (presented in a companion paper) with stacked CO limits from galaxies with available spectroscopic redshifts (slit or mask spectroscopy from Keck and grism spectroscopy from HST) to give first blind constraints on high-z CO luminosity functions and the cosmic evolution of the H2 mass density $\rho_{\rm H2}$(z) out to redshifts z~3. A comparison to empirical predictions of $\rho_{\rm H2}$(z) shows that the securely detected sources in our molecular line scan already provide significant contributions to the predicted $\rho_{\rm H2}$(z) in the redshift bins ~1.5 and ~2.7. Accounting for galaxies with CO luminosities that are not probed by our observations results in cosmic molecular gas densities $\rho_{\rm H2}$(z) that are higher than current predictions. We note however that the current uncertainties (in particular the luminosity limits, number of detections, as well as cosmic volume probed) are significant, a situation that is about to change with the emerging ALMA observatory., Comment: Accepted for publication in ApJ
Published: 2013
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107. A molecular line scan in the Hubble Deep Field North

Author: Decarli, R., Walter, F., Carilli, C., Riechers, D., Cox, P., Neri, R., Aravena, M., Bell, E., Bertoldi, F., Colombo, D., Da Cunha, E., Daddi, E., Dickinson, M., Downes, D., Ellis, R., Lentati, L., Maiolino, R., Menten, K. M., Rix, H. W., Sargent, M., Stark, D., Weiner, B., and Weiss, A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a molecular line scan in the Hubble Deep Field North (HDF-N) that covers the entire 3mm window (79-115 GHz) using the IRAM Plateau de Bure Interferometer. Our CO redshift coverage spans z<0.45, 12. We reach a CO detection limit that is deep enough to detect essentially all z>1 CO lines reported in the literature so far. We have developed and applied different line searching algorithms, resulting in the discovery of 17 line candidates. We estimate that the rate of false positive line detections is ~2/17. We identify optical/NIR counterparts from the deep ancillary database of the HDF-N for seven of these candidates and investigate their available SEDs. Two secure CO detections in our scan are identified with star-forming galaxies at z=1.784 and at z=2.047. These galaxies have colors consistent with the `BzK' color selection and they show relatively bright CO emission compared with galaxies of similar dust continuum luminosity. We also detect two spectral lines in the submillimeter galaxy HDF850.1 at z=5.183. We consider an additional 9 line candidates as high quality. Our observations also provide a deep 3mm continuum map (1-sigma noise level = 8.6 $\mu$Jy/beam). Via a stacking approach, we find that optical/MIR bright galaxies contribute only to <50% of the SFR density at 1
Published: 2013
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108. An ALMA survey of sub-millimeter galaxies in the Extended Chandra Deep Field South: Sub-millimeter properties of color-selected galaxies

Author: Decarli, R., Smail, I., Walter, F., Swinbank, A. M., Chapman, S., Coppin, K. E. K., Cox, P., Dannerbauer, H., Greve, T. R., Hodge, J. A., Ivison, R., Karim, A., Knudsen, K. K., Lindroos, L., Rix, H. -W., Schinnerer, E., Simpson, J. M., van der Werf, P., and Weiss, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the sub-mm properties of color-selected galaxies via a stacking analysis applied for the first time to interferometric data at sub-mm wavelengths. We base our study on 344 GHz ALMA continuum observations of ~20''-wide fields centered on 86 sub-mm sources detected in the LABOCA Extended Chandra Deep Field South Sub-mm Survey (LESS). We select various classes of galaxies (K-selected, star-forming sBzK galaxies, extremely red objects and distant red galaxies) according to their optical/NIR fluxes. We find clear, >10-sigma detections in the stacked images of all these galaxy classes. We include in our stacking analysis Herschel/SPIRE data to constrain the dust SED of these galaxies. We find that their dust emission is well described by a modified black body with Tdust~30 K and beta=1.6 and IR luminosities of (5-11)x10^{11} Lsun, or implied star formation rates of 75-140 Msun/yr. We compare our results with those of previous studies based on single-dish observations at 870 micron and find that our flux densities are a factor 2-3 higher than previous estimates. The discrepancy is observed also after removing sources individually detected in ALESS maps. We report a similar discrepancy by repeating our analysis on 1.4\,GHz observations of the whole ECDFS. Hence we find tentative evidence that galaxies that are associated in projected and redshift space with sub-mm bright sources are brighter than the average population. Finally, we put our findings in the context of the cosmic star formation rate density as a function of redshift., Comment: 9 figures. Accepted for publication in ApJ
Published: 2013
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109. A Search for Planetary Nebulae With the SDSS: the outer regions of M31

Author: Kniazev, A. Y., Grebel, E. K., Zucker, D. B., Rix, H-W., Martinez-Delgado, D., and Snedden, S. A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have developed a method to identify planetary nebula (PN) candidates in imaging data of the Sloan Digital Sky Survey (SDSS). This method exploits the SDSS' five-band sampling of emission lines in PN spectra, which results in a color signature distinct from that of other sources. Selection criteria based on this signature can be applied to nearby galaxies in which PNe appear as point sources. We applied these criteria to the whole area of M31 as scanned by the SDSS, selecting 167 PN candidates that are located in the outer regions of M31. The spectra of 80 selected candidates were then observed with the 2.2m telescope at Calar Alto Observatory. These observations and cross-checks with literature data show that our method has a selection rate efficiency of about 90%, but the efficiency is different for the different groups of PNe candidates. In the outer regions of M31, PNe trace different well-known morphological features like the Northern Spur, the NGC205 Loop, the G1 Clump, etc. In general, the distribution of PNe in the outer region 8
Published: 2013
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110. Discovery of a Quadruple Lens in CANDELS with a Record Lens Redshift z=1.53

Author: van der Wel, A., van de Ven, G., Maseda, M., Rix, H. W., Rudnick, G. H., Grazian, A., Finkelstein, S. L., Koo, D. C., Faber, S. M., Ferguson, H. C., Koekemoer, A. M., Grogin, N. A., and Kocevski, D. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using spectroscopy from the Large Binocular Telescope and imaging from the Hubble Space Telescope we discovered the first strong galaxy lens at z(lens)>1. The lens has a secure photometric redshift of z=1.53+/-0.09 and the source is spectroscopically confirmed at z=3.417. The Einstein radius (0.35"; 3.0 kpc) encloses 7.6 x 10^10 Msol, with an upper limit on the dark matter fraction of 60%. The highly magnified (40x) source galaxy has a very small stellar mass (~10^8 Msol) and shows an extremely strong [OIII]_5007A emission line (EW_0 ~ 1000A) bolstering the evidence that intense starbursts among very low-mass galaxies are common at high redshift., Comment: accepted for publication in ApJ Letters
Published: 2013
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111. Complete infrared spectral energy distributions of mm detected quasars at z>5

Author: Leipski, C., Meisenheimer, K., Walter, F., Besel, M. -A., Dannerbauer, H., Fan, X., Haas, M., Klaas, U., Krause, O., and Rix, H. -W.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel far-infrared (FIR) photometry of eleven quasars at redshift z>5 that have previously been detected at 1.2mm. We perform full spectral energy distribution (SED) fits over the wavelength range lambda_rest ~0.1-400mu for those objects with good Herschel detections. These fits reveal the need for an additional far-infrared (FIR) component besides the emission from a dusty AGN-powered torus. This additional FIR component has temperatures of T_FIR ~ 40-60K with luminosities of L_(8-1000mu) ~ 10^13 L_sun (accounting for 25-60% of the bolometric FIR luminosity). If the FIR dust emission is due to star formation it would suggest star formation rates in excess of 1000 solar masses per year. We show that at long wavelengths (lambda_rest > 50mu) the contribution of the AGN-powered torus emission is negligible. This explains how previous FIR studies of high-redshift quasars that relied on single component fits to (ground-based) observations at lambda_obs > 350mu reached T_FIR and L_FIR values similar to our complete SED fits. Stacking the Herschel data of four individually undetected sources reveals a significant average signal in the PACS bands but not in SPIRE. The average SED of sources with individual Herschel detections shows a striking surplus in near- and mid-infrared emission when compared to common AGN templates. The comparison between two average SEDs (sources with and without individual Herschel detections) matched in the UV/optical indicates that for these objects the strength of the MIR emission may correlate with the strength of the FIR emission., Comment: 15 pages, 7 figures, accepted for publication in ApJ
Published: 2013
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112. An ALMA survey of submillimeter galaxies in the Extended Chandra Deep Field South: Source catalog and multiplicity

Author: Hodge, J. A., Karim, A., Smail, I., Swinbank, A. M., Walter, F., Biggs, A. D., Ivison, R. J., Weiss, A., Alexander, D. M., Bertoldi, F., Brandt, W. N., Chapman, S. C., Coppin, K. E. K., Cox, P., Danielson, A. L. R., Dannerbauer, H., De Breuck, C., Decarli, R., Edge, A. C., Greve, T. R., Knudsen, K. K., Menten, K. M., Rix, H. -W., Schinnerer, E., Simpson, J. M., Wardlow, J. L., and van der Werf, P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 0 survey of 126 submillimeter sources from the LABOCA ECDFS Submillimeter Survey (LESS). Our 870 micron survey with ALMA (ALESS) has produced maps ~3X deeper and with a beam area ~200X smaller than the original LESS observations, doubling the current number of interferometrically-observed submillimeter sources. The high resolution of these maps allows us to resolve sources that were previously blended and accurately identify the origin of the submillimeter emission. We discuss the creation of the ALESS submillimeter galaxy (SMG) catalog, including the main sample of 99 SMGs and a supplementary sample of 32 SMGs. We find that at least 35% (possibly up to 50%) of the detected LABOCA sources have been resolved into multiple SMGs, and that the average number of SMGs per LESS source increases with LESS flux density. Using the (now precisely known) SMG positions, we empirically test the theoretical expectation for the uncertainty in the single-dish source positions. We also compare our catalog to the previously predicted radio/mid-infrared counterparts, finding that 45% of the ALESS SMGs were missed by this method. Our ~1.6" resolution allows us to measure a size of ~9 kpc X 5 kpc for the rest-frame ~300 um emission region in one resolved SMG, implying a star formation rate surface density of 80 M_sol yr^-1 kpc^-2, and we constrain the emission regions in the remaining SMGs to be <10 kpc. As the first statistically reliable survey of SMGs, this will provide the basis for an unbiased multiwavelength study of SMG properties., Comment: To appear in ApJ
Published: 2013
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113. A Detailed Study of the Radio--FIR Correlation in NGC6946 with Herschel-PACS/SPIRE from KINGFISH

Author: Tabatabaei, F. S., Schinnerer, E., Murphy, E. J., Beck, R., Groves, B., Meidt, S., Krause, M., Rix, H-W., Sandstrom, K., Crocker, A. F., Galametz, M., Helou, G., Wilson, C. D., Kennicutt, R., Calzetti, D., Draine, B., Aniano, G., Dale, D., Dumas, G., Engelbracht, C. W., Gordon, K. D., Hinz, J., Kreckel, K., Montiel, E., and Roussel, H.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We derive the distribution of the synchrotron spectral index across NGC6946 and investigate the correlation between the radio continuum (synchrotron) and far-infrared (FIR) emission using the KINGFISH Herschel PACS and SPIRE data. The radio--FIR correlation is studied as a function of star formation rate, magnetic field strength, radiation field strength, and the total gas surface brightness. The synchrotron emission follows both star-forming regions and the so-called magnetic arms present in the inter-arm regions. The synchrotron spectral index is steepest along the magnetic arms ($\alpha_n \sim 1$), while it is flat in places of giant H{\sc ii} regions and in the center of the galaxy ($\alpha_n \sim 0.6-0.7$). The map of $\alpha_n$ provides an observational evidence for aging and energy loss of cosmic ray electrons propagating in the disk of the galaxy. Variations in the synchrotron--FIR correlation across the galaxy are shown to be a function of both star formation and magnetic fields. We find that the synchrotron emission correlates better with cold rather than with warm dust emission, when the interstellar radiation field is the main heating source of dust. The synchrotron--FIR correlation suggests a coupling between the magnetic field and the gas density. NGC6946 shows a power-law behavior between the total (turbulent) magnetic field strength B and the star formation rate surface density $\Sigma_{\rm SFR}$ with an index of 0.14\,(0.16)$\pm$0.01. This indicates an efficient production of the turbulent magnetic field with the increasing gas turbulence expected in actively star forming regions. The scale-by-scale analysis of the synchrotron--FIR correlation indicates that the ISM affects the propagation of old/diffused cosmic ray electrons, resulting in a diffusion coefficient of $D_0=4.6\times 10^{28}$\,cm$^2$\,s$^{-1}$ for 2.2\,GeV CREs., Comment: 23 pages, 13 figures, accepted for publication in Astronomy & Astrophysics Journal
Published: 2013
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114. MaGICC Thick Disk I: Comparing a Simulated Disk Formed with Stellar Feedback to the Milky Way

Author: Stinson, G. S., Bovy, J., Rix, H. -W., Brook, C., Roškar, R., Dalcanton, J. J., Macciò, A. V., Wadsley, J., Couchman, H. M. P., and Quinn, T. R.
Subjects: Astrophysics - Galaxy Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We analyse the structure and chemical enrichment of a Milky Way-like galaxy with a stellar mass of 2 10^{10} M_sun, formed in a cosmological hydrodynamical simulation. It is disk-dominated with a flat rotation curve, and has a disk scale length similar to the Milky Way's, but a velocity dispersion that is ~50% higher. Examining stars in narrow [Fe/H] and [\alpha/Fe] abundance ranges, we find remarkable qualitative agreement between this simulation and observations: a) The old stars lie in a thickened distribution with a short scale length, while the young stars form a thinner disk, with scale lengths decreasing, as [Fe/H] increases. b) Consequently, there is a distinct outward metallicity gradient. c) Mono-abundance populations exist with a continuous distribution of scale heights (from thin to thick). However, the simulated galaxy has a distinct and substantive very thick disk (h_z~1.5 kpc), not seen in the Milky Way. The broad agreement between simulations and observations allows us to test the validity of observational proxies used in the literature: we find in the simulation that mono-abundance populations are good proxies for single age populations (<1 Gyr) for most abundances., Comment: 11 page, 10 figures, submitted. Comments welcome
Published: 2013
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115. The CO-to-H2 Conversion Factor and Dust-to-Gas Ratio on Kiloparsec Scales in Nearby Galaxies

Author: Sandstrom, K. M., Leroy, A. K., Walter, F., Bolatto, A. D., Croxall, K. V., Draine, B. T., Wilson, C. D., Wolfire, M., Calzetti, D., Kennicutt, R. C., Aniano, G., Meyer, J. Donovan, Usero, A., Bigiel, F., Brinks, E., de Blok, W. J. G, Crocker, A., Dale, D., Engelbracht, C. W., Galametz, M., Groves, B., Hunt, L. K., Koda, J., Kreckel, K., Linz, H., Meidt, S., Pellegrini, E., Rix, H. -W., Roussel, H., Schinnerer, E., Schruba, A., Schuster, K. -F., Skibba, R., van der Laan, T., Appleton, P., Armus, L., Brandl, B., Gordon, K., Hinz, J., Krause, O., Montiel, E., Sauvage, M., Schmiedeke, A., Smith, J. D. T., and Vigroux, L.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present kiloparsec (kpc) spatial resolution maps of the CO-to-H2 conversion factor (alpha_co) and dust-to-gas ratio (DGR) in 26 nearby, star-forming galaxies. We have simultaneously solved for alpha_co and DGR by assuming that the DGR is approximately constant on kpc scales. With this assumption, we can combine maps of dust mass surface density, CO integrated intensity and HI column density to solve for both alpha_co and DGR with no assumptions about their value or dependence on metallicity or other parameters. Such a study has just become possible with the availability of high resolution far-IR maps from the Herschel key program KINGFISH, 12CO J=(2-1) maps from the IRAM 30m large program HERACLES and HI 21-cm line maps from THINGS. We use a fixed ratio between the (2-1) and (1-0) lines to present our alpha_co results on the more typically used 12CO J=(1-0) scale and show using literature measurements that variations in the line ratio do not effect our results. In total, we derive 782 individual solutions for alpha_co and DGR. On average, alpha_co = 3.1 Msun pc^-2 (K km s^-1)^-1 for our sample with a standard deviation of 0.3 dex. Within galaxies we observe a generally flat profile of alpha_co as a function of galactocentric radius. However, most galaxies exhibit a lower alpha_co in the central kpc---a factor of ~2 below the galaxy mean, on average. In some cases, the central alpha_co value can be factors of 5 to 10 below the standard Milky Way (MW) value of alpha_co,MW =4.4 Msun pc^-2 (K km s^-1)^-1. While for alpha_co we find only weak correlations with metallicity, DGR is well-correlated with metallicity, with an approximately linear slope. Finally, we present several recommendations for choosing an appropriate alpha_co for studies of nearby galaxies., Comment: accepted to ApJ July 9, 2013, 63 pages, 2-column ApJ format, p38-63 are an image atlas
Published: 2012
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116. Structural Parameters of Galaxies in CANDELS

Author: van der Wel, A., Bell, E. F., Haussler, B., McGrath, E. J., Chang, Yu-Yen, Guo, Yicheng, McIntosh, D. H., Rix, H. -W., Barden, M., Cheung, E., Faber, S. M., Ferguson, H. C., Galametz, A., Grogin, N. A., Hartley, W., Kartaltepe, J. S., Kocevski, D. D., Koekemoer, A. M., Lotz, J., Mozena, M., Peth, M. A., and Peng, Chien Y.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We present global structural parameter measurements of 109,533 unique, H_F160W-selected objects from the CANDELS multi-cycle treasury program. Sersic model fits for these objects are produced with GALFIT in all available near-infrared filters (H_F160W, J_F125W and, for a subset, Y_F105W). The parameters of the best-fitting Sersic models (total magnitude, half-light radius, Sersic index, axis ratio, and position angle) are made public, along with newly constructed point spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements -- to 10% or better -- of all structural parameters can typically be obtained for galaxies with H_F160W < 23, with comparable fidelity for basic size and shape measurements for galaxies to H_F160W ~ 24.5., Comment: public data release of structural parameters from CANDELS WFC3 data: http://www.mpia-hd.mpg.de/homes/vdwel/candels.html
Published: 2012
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117. Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: NGC 628 and NGC 6946

Author: Aniano, G., Draine, B. T., Calzetti, D., Dale, D. A., Engelbracht, C. W., Gordon, K. D., Hunt, L. K., Kennicutt, R. C., Krause, O., Leroy, A. K., Rix, H-W., Roussel, H., Sandstrom, K., Sauvage, M., Walter, F., Armus, L., Bolatto, A. D., Crocker, A., Meyer, J. Donovan, Galametz, M., Helou, G., Hinz, J., Johnson, B. D., Koda, J., Montiel, E., Murphy, E. J., Skibba, R., Smith, J. -D. T., and Wolfire, M. G.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We characterize the dust in NGC628 and NGC6946, two nearby spiral galaxies in the KINGFISH sample. With data from 3.6um to 500um, dust models are strongly constrained. Using the Draine & Li (2007) dust model, (amorphous silicate and carbonaceous grains), for each pixel in each galaxy we estimate (1) dust mass surface density, (2) dust mass fraction contributed by polycyclic aromatic hydrocarbons (PAH)s, (3) distribution of starlight intensities heating the dust, (4) total infrared (IR) luminosity emitted by the dust, and (5) IR luminosity originating in regions with high starlight intensity. We obtain maps for the dust properties, which trace the spiral structure of the galaxies. The dust models successfully reproduce the observed global and resolved spectral energy distributions (SEDs). The overall dust/H mass ratio is estimated to be 0.0082+/-0.0017 for NGC628, and 0.0063+/-0.0009 for NGC6946, consistent with what is expected for galaxies of near-solar metallicity. Our derived dust masses are larger (by up to a factor 3) than estimates based on single-temperature modified blackbody fits. We show that the SED fits are significantly improved if the starlight intensity distribution includes a (single intensity) "delta function" component. We find no evidence for significant masses of cold dust T<12K. Discrepancies between PACS and MIPS photometry in both low and high surface brightness areas result in large uncertainties when the modeling is done at PACS resolutions, in which case SPIRE, MIPS70 and MIPS160 data cannot be used. We recommend against attempting to model dust at the angular resolution of PACS., Comment: To be published in Apj, September 2012. See the full version at http://www.astro.princeton.edu/~ganiano/Papers/
Published: 2012
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118. The Intense Starburst HDF850.1 in a Galaxy Overdensity at z=5.2 in the Hubble Deep Field

Author: Walter, Fabian, Decarli, R., Carilli, C., Bertoldi, F., Cox, P., Da Cunha, E., Daddi, E., Dickinson, M., Downes, D., Elbaz, D., Ellis, R., Hodge, J., Neri, R., Riechers, D., Weiss, A., Bell, E., Dannerbauer, H., Krips, M., Krumholz, M., Lentati, L., Maiolino, R., Menten, K., Rix, H. -W., Robertson, B., Spinrad, H., Stark, D., and Stern, D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Hubble Deep Field (HDF) is a region in the sky that provides one of the deepest multi-wavelength views of the distant universe and has led to the detection of thousands of galaxies seen throughout cosmic time. An early map of the HDF at a wavelength of 850 microns that is sensitive to dust emission powered by star formation revealed the brightest source in the field, dubbed HDF850.1. For more than a decade, this source remained elusive and, despite significant efforts, no counterpart at shorter wavelengths, and thus no redshift, size or mass, could be identified. Here we report, using a millimeter wave molecular line scan, an unambiguous redshift determination for HDF850.1 of z=5.183. This places HDF850.1 in a galaxy overdensity at z~5.2 in the HDF, corresponding to a cosmic age of only 1.1 Gyr after the Big Bang. This redshift is significantly higher than earlier estimates and higher than most of the >100 sub-millimeter bright galaxies identified to date. The source has a star formation rate of 850 M_sun/yr and is spatially resolved on scales of 5 kpc, with an implied dynamical mass of ~1.3x10^11 M_sun, a significant fraction of which is present in the form of molecular gas. Despite our accurate redshift and position, a counterpart arising from starlight remains elusive., Comment: Nature, in press
Published: 2012
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119. A Study of Heating and Cooling of the ISM in NGC 1097 with Herschel-PACS and Spitzer-IRS

Author: Beirao, P., Armus, L., Helou, G., Appleton, P. N., Smith, J. -D. T., Croxall, K. V., Murphy, E. J., Dale, D. A., Draine, B. T., Wolfire, M. G., Sandstrom, K. M., Aniano, G., Bolatto, A. D., Groves, B., Brandl, B. R., Schinnerer, E., Crocker, A. F., Hinz, J. L., Rix, H. -W., Kennicutt, R. C., Calzetti, D., de Paz, A. Gil, Dumas, G., Galametz, M., Gordon, K. D., Hao, C. -N., Johnson, B., Koda, J., Krause, O., van der Laan, T., Leroy, A. K., Li, Y., Meidt, S. E., Meyer, J. D., Rahman, N., Roussel, H., Sauvage, M., Srinivasan, S., Vigroux, L., Walter, F., and Warren, B. E.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst ring, a strong large-scale bar and an active nucleus. We present a detailed study of the spatial variation of the far infrared (FIR) [CII]158um and [OI]63um lines and mid-infrared H2 emission lines as tracers of gas cooling, and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the photoelectric heating, using Herschel-PACS, and Spitzer-IRS infrared spectral maps. We focus on the nucleus and the ring, and two star forming regions (Enuc N and Enuc S). We estimated a photoelectric gas heating efficiency ([CII]158um+[OI]63um)/PAH in the ring about 50% lower than in Enuc N and S. The average 11.3/7.7um PAH ratio is also lower in the ring, which may suggest a larger fraction of ionized PAHs, but no clear correlation with [CII]158{\mu}m/PAH(5.5 - 14um) is found. PAHs in the ring are responsible for a factor of two more [CII]158um and [OI]63um emission per unit mass than PAHs in the Enuc S. SED modeling indicates that at most 25% of the FIR power in the ring and Enuc S can come from high intensity photodissociation regions (PDRs), in which case G0 ~ 10^2.3 and nH ~ 10^3.5 cm^-3 in the ring. For these values of G0 and nH PDR models cannot reproduce the observed H2 emission. Much of the the H2 emission in the starburst ring could come from warm regions in the diffuse ISM that are heated by turbulent dissipation or shocks., Comment: 17 pages, 14 figures, 5 tables; accepted for publication in ApJ
Published: 2012
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120. The Panchromatic Hubble Andromeda Treasury

Author: Dalcanton, J. J., Williams, B. F., Lang, D., Lauer, T. R., Kalirai, J. S., Seth, A. C., Dolphin, A., Rosenfield, P., Weisz, D. R., Bell, E. F., Bianchi, L. C., Boyer, M. L., Caldwell, N., Dong, H., Dorman, C. E., Gilbert, K. M., Girardi, L., Gogarten, S. M., Gordon, K. D., Guhathakurta, P., Hodge, P. W., Holtzman, J. A., Johnson, L., Larsen, S. S., Lewis, A., Melbourne, J. L., Olsen, K. A. G., Rix, H. -W., Rosema, K., Saha, A., Sarajedini, A., Skillman, E. D., and Stanek, K. Z.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: The Panchromatic Hubble Andromeda Treasury (PHAT) is an on-going HST Multicycle Treasury program to image ~1/3 of M31's star forming disk in 6 filters, from the UV to the NIR. The full survey will resolve the galaxy into more than 100 million stars with projected radii from 0-20 kpc over a contiguous 0.5 square degree area in 828 orbits, producing imaging in the F275W and F336W filters with WFC3/UVIS, F475W and F814W with ACS/WFC, and F110W and F160W with WFC3/IR. The resulting wavelength coverage gives excellent constraints on stellar temperature, bolometric luminosity, and extinction for most spectral types. The photometry reaches SNR=4 at F275W=25.1, F336W=24.9, F475W=27.9, F814W=27.1, F110W=25.5, and F160W=24.6 for single pointings in the uncrowded outer disk; however, the optical and NIR data are crowding limited, and the deepest reliable magnitudes are up to 5 magnitudes brighter in the inner bulge. All pointings are dithered and produce Nyquist-sampled images in F475W, F814W, and F160W. We describe the observing strategy, photometry, astrometry, and data products, along with extensive tests of photometric stability, crowding errors, spatially-dependent photometric biases, and telescope pointing control. We report on initial fits to the structure of M31's disk, derived from the density of RGB stars, in a way that is independent of the assumed M/L and is robust to variations in dust extinction. These fits also show that the 10 kpc ring is not just a region of enhanced recent star formation, but is instead a dynamical structure containing a significant overdensity of stars with ages >1 Gyr. (Abridged), Comment: 48 pages including 22 pages of figures. Accepted to the Astrophysical Journal Supplements. Some figures slightly degraded to reduce submission size
Published: 2012
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121. Photometric Calibration of the First 1.5 Years of the Pan-STARRS1 Survey

Author: Schlafly, E. F., Finkbeiner, D. P., Juric, M., Magnier, E. A., Burgett, W. S., Chambers, K. C., Grav, T., Hodapp, K. W., Kaiser, N., Kudritzki, R. -P., Martin, N. F., Morgan, J. S., Price, P. A., Rix, H. -W., Stubbs, C. W., Tonry, J. L., and Wainscoat, R. J.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present a precise photometric calibration of the first 1.5 years of science imaging from the Pan-STARRS1 survey (PS1), an ongoing optical survey of the entire sky north of declination -30 degrees in five bands. Building on the techniques employed by Padmanabhan et al. (2008) in the Sloan Digital Sky Survey (SDSS), we use repeat PS1 observations of stars to perform the relative calibration of PS1 in each of its five bands, solving simultaneously for the system throughput, the atmospheric transparency, and the large-scale detector flat field. Both internal consistency tests and comparison against the SDSS indicate that we achieve relative precision of <10 mmag in g, r, and i_P1, and ~10 mmag in z and y_P1. The spatial structure of the differences with the SDSS indicates that errors in both the PS1 and SDSS photometric calibration contribute similarly to the differences. The analysis suggests that both the PS1 system and the Haleakala site will enable <1% photometry over much of the sky., Comment: 16 pages, 9 figures (arxiv version updated to published version)
Published: 2012
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122. Resolving the Far-IR Line Deficit: Photoelectric Heating and Far-IR Line Cooling in NGC 1097 and NGC 4559

Author: Croxall, Kevin V., Smith, J. D., Wolfire, M. G., Roussel, H., Sandstrom, K. M., Draine, B. T., Aniano, G., Dale, D. A., Armus, L., Beirão, P., Helou, G., Bolatto, A. D., Appleton, P. N., Brandl, B. R., Calzetti, D., Crocker, A. F., Galametz, M., Groves, B. A., Hao, C. N., Hunt, L. K., Johnson, B. D., Kennicutt, R. C., Koda, J., Krause, O., Li, Y., Meidt, S. E., Murphy, E. J., Rahman, N., Rix, H. -W., Sauvage, M., Schinnerer, E., Walter, F., and Wilson, C. D.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The physical state of interstellar gas and dust is dependent on the processes which heat and cool this medium. To probe heating and cooling of the ISM over a large range of infrared surface brightness, on sub-kiloparsec scales, we employ line maps of [C \ii] 158 $\mu$m, [O \one] 63 $\mu$m, and [N \ii] 122 $\mu$m in NGC 1097 and NGC 4559, obtained with the PACS spectrometer onboard {\it Herschel}. We matched new observations to existing Spitzer-IRS data that trace the total emission of polycyclic aromatic hydrocarbons (PAHs). We confirm at small scales in these galaxies that the canonical measure of photoelectric heating efficiency, ([C \ii] + [O \one])/TIR, decreases as the far-infrared color, $\nu f_\nu$(70 $\mu$m)/$\nu f_\nu$(100 $\mu$m), increases. In contrast, the ratio of far-infrared (far-IR) cooling to total PAH emission, ([C \ii] + [O \one])/PAH, is a near constant $\sim$6% over a wide range of far-infrared color, 0.5 \textless\ $\nu f_\nu$(70 $\mu$m)/$\nu f_\nu$(100 $\mu$m) $\lesssim$ 0.95. In the warmest regions, where $\nu f_\nu$(70 $\mu$m)/$\nu f_\nu$(100 $\mu$m) $\gtrsim$ 0.95, the ratio ([C \ii] + [O \one])/PAH drops rapidly to 4%. We derived representative values of the local UV radiation density, $G_0$, and the gas density, $n_H$, by comparing our observations to models of photodissociation regions. The ratio $G_0/n_H$, derived from fine-structure lines, is found to correlate with the mean dust-weighted starlight intensity, $$ derived from models of the IR SED. Emission from regions that exhibit a line deficit is characterized by an intense radiation field, indicating that small grains are susceptible to ionization effects. We note that there is a shift in the 7.7 / 11.3 $\mu$m PAH ratio in regions that exhibit a deficit in ([C \ii] + [O \one])/PAH, suggesting that small grains are ionized in these environments., Comment: 19 pages, 14 pages, accepted for publication in ApJ
Published: 2012
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123. Herschel Far-Infrared and Sub-millimeter Photometry for the KINGFISH Sample of Nearby Galaxies

Author: Dale, D. A., Aniano, G., Engelbracht, C. W., Hinz, J. L., Krause, O., Montiel, E. J., Roussel, H., Appleton, P. N., Armus, L., Beirao, P., Bolatto, A. D., Brandl, B. R., Calzetti, D., Crocker, A. F., Croxall, K. V., Draine, B. T., Galametz, M., Gordon, K. D., Groves, B. A., Hao, C. -N., Helou, G., Hunt, L. K., Johnson, B. D., Kennicutt, R. C., Koda, J., Leroy, A. K., Li, Y., Meidt, S. E., Miller, A. E., Murphy, E. J., Rahman, N., Rix, H. -W., Sandstrom, K. M., Sauvage, M., Schinnerer, E., Skibba, R. A., Smith, J. -D. T., Tabatabaei, F. S., Walter, F., Wilson, C. D., Wolfire, M. G., and Zibetti, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: New far-infrared and sub-millimeter photometry from the Herschel Space Observatory is presented for 61 nearby galaxies from the Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel (KINGFISH) sample. The spatially-integrated fluxes are largely consistent with expectations based on Spitzer far-infrared photometry and extrapolations to longer wavelengths using popular dust emission models. Dwarf irregular galaxies are notable exceptions, as already noted by other authors, as their 500um emission shows evidence for a sub-millimeter excess. In addition, the fraction of dust heating attributed to intense radiation fields associated with photo-dissociation regions is found to be (21+/-4)% larger when Herschel data are included in the analysis. Dust masses obtained from the dust emission models of Draine & Li are found to be on average nearly a factor of two higher than those based on single-temperature modified blackbodies, as single blackbody curves do not capture the full range of dust temperatures inherent to any galaxy. The discrepancy is largest for galaxies exhibiting the coolest far-infrared colors., Comment: Accepted for publication in ApJ
Published: 2011
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124. KINGFISH -- Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel: Survey Description and Image Atlas

Author: Kennicutt, R. C., Calzetti, D., Aniano, G., Appleton, P., Armus, L., Beirao, P., Bolatto, A. D., Brandl, B., Crocker, A., Croxall, K., Dale, D. A., Meyer, J. Dononvan, Draine, B. T., Engelbracht, C. W., Galametz, M., Gordon, K. D., Groves, B., Hao, C. -N., Helou, G., Hinz, J., Hunt, L. K., Johnson, B., Koda, J., Krause, O., Leroy, A. K., Li, Y., Meidt, S., Montiel, E., Murphy, E. J., Rahman, N., Rix, H. -W., Roussel, H., Sandstrom, K., Sauvage, M., Schinnerer, E., Skibba, R., Smith, J. -D. T., Srinivasan, S., Vigroux, L., Walter, F., Wilson, C. D., Wolfire, M., and Zibetti, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The KINGFISH project (Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel) is an imaging and spectroscopic survey of 61 nearby (d < 30 Mpc) galaxies, chosen to cover a wide range of galaxy properties and local interstellar medium (ISM) environments found in the nearby Universe. Its broad goals are to characterize the ISM of present-day galaxies, the heating and cooling of their gaseous and dust components, and to better understand the physical processes linking star formation and the ISM. KINGFISH is a direct descendant of the Spitzer Infrared Nearby Galaxies Survey (SINGS), which produced complete Spitzer imaging and spectroscopic mapping and a comprehensive set of multi-wavelength ancillary observations for the sample. The Herschel imaging consists of complete maps for the galaxies at 70, 100, 160, 250, 350, and 500 microns. The spectal line imaging of the principal atomic ISM cooling lines ([OI]63um, [OIII]88um, [NII]122,205um, and [CII]158um) covers the subregions in the centers and disks that already have been mapped in the mid-infrared with Spitzer. The KINGFISH and SINGS multi-wavelength datasets combined provide panchromatic mapping of the galaxies sufficient to resolve individual star-forming regions, and tracing the important heating and cooling channels of the ISM, across a wide range of local extragalactic ISM environments. This paper summarizes the scientific strategy for KINGFISH, the properties of the galaxy sample, the observing strategy, and data processing and products. It also presents a combined Spitzer and Herschel image atlas for the KINGFISH galaxies, covering the wavelength range 3.6 -- 500 microns. All imaging and spectroscopy data products will be released to the Herschel user generated product archives., Comment: 52 pages, 10 figures, 2 tables. Accepted for publication in PASP. A pdf copy of the image atlas can be downloaded separately at the KINGFISH public website, http://www.ast.cam.ac.uk/sites/default/files/Kingfish_reduced.pdf
Published: 2011
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125. Euclid Definition Study Report

Author: Laureijs, R., Amiaux, J., Arduini, S., Auguères, J. -L., Brinchmann, J., Cole, R., Cropper, M., Dabin, C., Duvet, L., Ealet, A., Garilli, B., Gondoin, P., Guzzo, L., Hoar, J., Hoekstra, H., Holmes, R., Kitching, T., Maciaszek, T., Mellier, Y., Pasian, F., Percival, W., Rhodes, J., Criado, G. Saavedra, Sauvage, M., Scaramella, R., Valenziano, L., Warren, S., Bender, R., Castander, F., Cimatti, A., Fèvre, O. Le, Kurki-Suonio, H., Levi, M., Lilje, P., Meylan, G., Nichol, R., Pedersen, K., Popa, V., Lopez, R. Rebolo, Rix, H. -W., Rottgering, H., Zeilinger, W., Grupp, F., Hudelot, P., Massey, R., Meneghetti, M., Miller, L., Paltani, S., Paulin-Henriksson, S., Pires, S., Saxton, C., Schrabback, T., Seidel, G., Walsh, J., Aghanim, N., Amendola, L., Bartlett, J., Baccigalupi, C., Beaulieu, J. -P., Benabed, K., Cuby, J. -G., Elbaz, D., Fosalba, P., Gavazzi, G., Helmi, A., Hook, I., Irwin, M., Kneib, J. -P., Kunz, M., Mannucci, F., Moscardini, L., Tao, C., Teyssier, R., Weller, J., Zamorani, G., Osorio, M. R. Zapatero, Boulade, O., Foumond, J. J., Di Giorgio, A., Guttridge, P., James, A., Kemp, M., Martignac, J., Spencer, A., Walton, D., Blümchen, T., Bonoli, C., Bortoletto, F., Cerna, C., Corcione, L., Fabron, C., Jahnke, K., Ligori, S., Madrid, F., Martin, L., Morgante, G., Pamplona, T., Prieto, E., Riva, M., Toledo, R., Trifoglio, M., Zerbi, F., Abdalla, F., Douspis, M., Grenet, C., Borgani, S., Bouwens, R., Courbin, F., Delouis, J. -M., Dubath, P., Fontana, A., Frailis, M., Grazian, A., Koppenhöfer, J., Mansutti, O., Melchior, M., Mignoli, M., Mohr, J., Neissner, C., Noddle, K., Poncet, M., Scodeggio, M., Serrano, S., Shane, N., Starck, J. -L., Surace, C., Taylor, A., Verdoes-Kleijn, G., Vuerli, C., Williams, O. R., Zacchei, A., Altieri, B., Sanz, I. Escudero, Kohley, R., Oosterbroek, T., Astier, P., Bacon, D., Bardelli, S., Baugh, C., Bellagamba, F., Benoist, C., Bianchi, D., Biviano, A., Branchini, E., Carbone, C., Cardone, V., Clements, D., Colombi, S., Conselice, C., Cresci, G., Deacon, N., Dunlop, J., Fedeli, C., Fontanot, F., Franzetti, P., Giocoli, C., Garcia-Bellido, J., Gow, J., Heavens, A., Hewett, P., Heymans, C., Holland, A., Huang, Z., Ilbert, O., Joachimi, B., Jennins, E., Kerins, E., Kiessling, A., Kirk, D., Kotak, R., Krause, O., Lahav, O., van Leeuwen, F., Lesgourgues, J., Lombardi, M., Magliocchetti, M., Maguire, K., Majerotto, E., Maoli, R., Marulli, F., Maurogordato, S., McCracken, H., McLure, R., Melchiorri, A., Merson, A., Moresco, M., Nonino, M., Norberg, P., Peacock, J., Pello, R., Penny, M., Pettorino, V., Di Porto, C., Pozzetti, L., Quercellini, C., Radovich, M., Rassat, A., Roche, N., Ronayette, S., Rossetti, E., Sartoris, B., Schneider, P., Semboloni, E., Serjeant, S., Simpson, F., Skordis, C., Smadja, G., Smartt, S., Spano, P., Spiro, S., Sullivan, M., Tilquin, A., Trotta, R., Verde, L., Wang, Y., Williger, G., Zhao, G., Zoubian, J., and Zucca, E.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - Galaxy Astrophysics
Abstract: Euclid is a space-based survey mission from the European Space Agency designed to understand the origin of the Universe's accelerating expansion. It will use cosmological probes to investigate the nature of dark energy, dark matter and gravity by tracking their observational signatures on the geometry of the universe and on the cosmic history of structure formation. The mission is optimised for two independent primary cosmological probes: Weak gravitational Lensing (WL) and Baryonic Acoustic Oscillations (BAO). The Euclid payload consists of a 1.2 m Korsch telescope designed to provide a large field of view. It carries two instruments with a common field-of-view of ~0.54 deg2: the visual imager (VIS) and the near infrared instrument (NISP) which contains a slitless spectrometer and a three bands photometer. The Euclid wide survey will cover 15,000 deg2 of the extragalactic sky and is complemented by two 20 deg2 deep fields. For WL, Euclid measures the shapes of 30-40 resolved galaxies per arcmin2 in one broad visible R+I+Z band (550-920 nm). The photometric redshifts for these galaxies reach a precision of dz/(1+z) < 0.05. They are derived from three additional Euclid NIR bands (Y, J, H in the range 0.92-2.0 micron), complemented by ground based photometry in visible bands derived from public data or through engaged collaborations. The BAO are determined from a spectroscopic survey with a redshift accuracy dz/(1+z) =0.001. The slitless spectrometer, with spectral resolution ~250, predominantly detects Ha emission line galaxies. Euclid is a Medium Class mission of the ESA Cosmic Vision 2015-2025 programme, with a foreseen launch date in 2019. This report (also known as the Euclid Red Book) describes the outcome of the Phase A study., Comment: 116 pages, with executive summary and table of contents
Published: 2011

126. The Photometric Classification Server for Pan-STARRS1

Author: Saglia, R. P., Tonry, J. L., Bender, R., Greisel, N., Seitz, S., Senger, R., Snigula, J., Phleps, S., Wilman, D., Bailer-Jones, C. A. L., Klement, R. J., Rix, H. -W., Smith, K., Green, P. J., Burgett, W. S., Chambers, K. C., Heasley, J. N., Kaiser, N., Magnier, E. A., Morgan, J. S., Price, P. A., Stubbs, C. W., and Wainscoat, R. J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Pan-STARRS1 survey is obtaining multi-epoch imaging in 5 bands (gps rps ips zps yps) over the entire sky North of declination -30deg. We describe here the implementation of the Photometric Classification Server (PCS) for Pan-STARRS1. PCS will allow the automatic classification of objects into star/galaxy/quasar classes based on colors, the measurement of photometric redshifts for extragalactic objects, and constrain stellar parameters for stellar objects, working at the catalog level. We present tests of the system based on high signal-to-noise photometry derived from the Medium Deep Fields of Pan-STARRS1, using available spectroscopic surveys as training and/or verification sets. We show that the Pan-STARRS1 photometry delivers classifications and photometric redshifts as good as the Sloan Digital Sky Survey (SDSS) photometry to the same magnitude limits. In particular, our preliminary results, based on this relatively limited dataset down to the SDSS spectroscopic limits and therefore potentially improvable, show that stars are correctly classified as such in 85% of cases, galaxies in 97% and QSOs in 84%. False positives are less than 1% for galaxies, ~19% for stars and ~28% QSOs. Moreover, photometric redshifts for 1000 luminous red galaxies up to redshift 0.5 are determined to 2.4% precision with just 0.4% catastrophic outliers and small (-0.5%) residual bias. PCS will create a value added catalog with classifications and photometric redshifts for eventually many millions sources., Comment: Replaced with version accepted for publication in ApJ
Published: 2011
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127. Extreme Emission Line Galaxies in CANDELS: Broad-Band Selected, Star-Bursting Dwarf Galaxies at z>1

Author: van der Wel, A., Straughn, A. N., Rix, H. -W., Finkelstein, S. L., Koekemoer, A. M., Weiner, B. J., Wuyts, S., Bell, E. F., Faber, S. M., Trump, J. R., Koo, D. C., Ferguson, H. C., Scarlata, C., Hathi, N. P., Dunlop, J. S., Newman, J. A., Dickinson, M., Jahnke, K., Salmon, B. W., de Mello, D. F., Kocevski, D. D., Lai, K., Grogin, N. A ., Rodney, S. A., Guo, Yicheng, McGrath, E. G., Lee, K. -S., Barro, G., Huang, K. -H., Riess, A. G., Ashby, M. L. N., and Willner, S. P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We identify an abundant population of extreme emission line galaxies (EELGs) at redshift z~1.7 in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) imaging from Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3). 69 EELG candidates are selected by the large contribution of exceptionally bright emission lines to their near-infrared broad-band magnitudes. Supported by spectroscopic confirmation of strong [OIII] emission lines -- with rest-frame equivalent widths ~1000\AA -- in the four candidates that have HST/WFC3 grism observations, we conclude that these objects are galaxies with 10^8 Msol in stellar mass, undergoing an enormous starburst phase with M_*/(dM_*/dt) of only ~15 Myr. These bursts may cause outflows that are strong enough to produce cored dark matter profiles in low-mass galaxies. The individual star formation rates and the co-moving number density (3.7x10^-4 Mpc^-3) can produce in ~4 Gyr much of the stellar mass density that is presently contained in 10^8-10^9 Msol dwarf galaxies. Therefore, our observations provide a strong indication that many or even most of the stars in present-day dwarf galaxies formed in strong, short-lived bursts, mostly at z>1., Comment: accepted for publication in ApJ; 10 pages; 6 figures; 1 table
Published: 2011
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128. A Constant Molecular Gas Depletion Time in Nearby Disk Galaxies

Author: Bigiel, F., Leroy, A. K., Walter, F., Brinks, E., de Blok, W. J. G., Kramer, C., Rix, H. W., Schruba, A., Schuster, K. F., Usero, A., and Wiesemeyer, H. W.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We combine new sensitive, wide-field CO data from the HERACLES survey with ultraviolet and infrared data from GALEX and Spitzer to compare the surface densities of H2, Sigma_H2, and recent star formation rate, Sigma_SFR, over many thousands of positions in 30 nearby disk galaxies. We more than quadruple the size of the galaxy sample compared to previous work and include targets with a wide range of galaxy properties. Even though the disk galaxies in this study span a wide range of properties, we find a strong and approximately linear correlation between Sigma_SFR and Sigma_H2 at our common resolution of 1kpc. This implies a roughly constant median H2 consumption time, tau_H2 = Sigma_H2 / Sigma_SFR, of ~2.35Gyr (including heavy elements) across our sample. At 1kpc resolution, there is only a weak correlation between Sigma_H2 and tau_H2 over the range Sigma_H2~5-100M_sun/pc^2, which is probed by our data. We compile a broad set of literature measurements that have been obtained using a variety of star formation tracers, sampling schemes and physical scales and show that overall, these data yield almost exactly the same results, although with more scatter. We interpret these results as strong, albeit indirect evidence that star formation proceeds in a uniform way in giant molecular clouds in the disks of spiral galaxies., Comment: Accepted for Publication in ApJL
Published: 2011
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129. A Planetary Companion around a Metal-Poor Star with Extragalactic Origin

Author: Setiawan, J., Klement, R., Henning, T., Rix, H. -W., Rochau, B., Schulze-Hartung, T., and Rodmann, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of a planetary companion around HIP 13044, a metal-poor star on the red Horizontal Branch. The detection is based on radial velocity observations with FEROS, a high-resolution spectrograph at the 2.2-m MPG/ESO telescope, located at ESO La Silla observatory in Chile. The periodic radial velocity variation of P = 16.2 days can be distinguished from the periods of the stellar activity indicators. We computed a minimum planetary mass of 1.25 MJup and an orbital semi-major axis of 0.116 AU for the planet. This discovery is unique in three aspects: First, it is the first planet detection around a star with a metallicity much lower than few percent of the solar value; second, the planet host star resides in a stellar evolutionary stage that is still unexplored in the exoplanet surveys; third, the star HIP 13044 belongs to one of the most significant stellar halo streams in the solar neighborhood, implying an extragalactic origin of the planetary system HIP 13044 in a disrupted former satellite of the Milky Way., Comment: Part of PlanetsbeyondMS/2010 proceedings http://arxiv.org/html/1011.6606
Published: 2011
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130. The Displaced Dusty ISM of NGC 3077: Tidal Stripping in the M 81 Triplet

Author: Walter, Fabian, Sandstrom, Karin, Aniano, G., Calzetti, D., Croxall, K., Dale, D. A., Draine, B. T., Engelbracht, C., Hinz, J., Kennicutt, R. C., Wolfire, M., Armus, L., Beirao, P., Bolatto, A. D., Brandl, B., Crocker, A., Galametz, M., Groves, B., Hao, C. -N., Helou, G., Hunt, L., Koda, J., Krause, O., Leroy, A., Meidt, S., Murphy, E. J., Rahman, N., Rix, H. -W., Roussel, H., Sauvage, M., Schinnerer, E., Skibba, R., Smith, J. D., Wilson, C. D., and Zibetti, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the detection of extended (~30 kpc^2) dust emission in the tidal \hi\ arm near NGC 3077 (member of the M\,81 triplet) using SPIRE on board Herschel. Dust emission in the tidal arm is typically detected where the \hi\ column densities are >10^21 cm^-2. The SPIRE band ratios show that the dust in the tidal arm is significantly colder (~13 K) than in NGC 3077 itself (~31 K), consistent with the lower radiation field in the tidal arm. The total dust mass in the tidal arm is ~1.8 x 10^6 M_sun (assuming beta=2), i.e. substantially larger than the dust mass associated with NGC 3077 (~2 x 10^5 M_sun). Where dust is detected, the dust-to-gas ratio is 6+/-3 x 10^-3, consistent within the uncertainties with what is found in NGC 3077 and nearby spiral galaxies with Galactic metallicities. The faint HII regions in the tidal arm can not be responsible for the detected enriched material and are not the main source of the dust heating in the tidal arm. We conclude that the interstellar medium (atomic HI, molecules and dust) in this tidal feature was pre-enriched and stripped off NGC 3077 during its recent interaction (~3 x 10^8 yr ago) with M 82 and M 81. This implies that interaction can efficiently remove heavy elements and enriched material (dust, molecular gas) from galaxies. As interactions were more frequent at large lookback times, it is conceivable that they could substantially contribute (along with galactic outflows) to the enrichment of the intergalactic medium., Comment: ApJ Letters, in print
Published: 2011
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131. Infrared Narrow-Band Tomography of the Local Starburst NGC 1569 with LBT/LUCIFER

Author: Pasquali, A., Bik, A., Zibetti, S., Ageorges, N., Seifert, W., Brandner, W., Rix, H. -W., Juette, M, Knierim, V., Buschkamp, P., Feiz, C., Gemperlein, H., Germeroth, A., Hoffmann, R., Laun, W., Lederer, R., Lehmitz, M., Lenzen, R., Mall, U., Mandel, H., Mueller, P., Naranjo, V., Polsterer, K., Quirrenbach, A., Schaeffner, L., Storz, C., and Weiser, P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We used the near-IR imager/spectrograph LUCIFER mounted on the Large Binocular Telescope (LBT) to image, with sub-arcsec seeing, the local dwarf starburst NGC 1569 in the JHK bands and HeI 1.08 micron, [FeII] 1.64 micron and Brgamma narrow-band filters. We obtained high-quality spatial maps of HeI, [FeII] and Brgamma emission across the galaxy, and used them together with HST/ACS images of NGC 1569 in the Halpha filter to derive the two-dimensional spatial map of the dust extinction and surface star formation rate density. We show that dust extinction is rather patchy and, on average, higher in the North-West (NW) portion of the galaxy [E_g(B-V) = 0.71 mag] than in the South-East [E_g(B-V) = 0.57 mag]. Similarly, the surface density of star formation rate peaks in the NW region of NGC 1569, reaching a value of about 4 x 10^-6 M_sun yr^-1 pc^-2. The total star formation rate as estimated from the integrated, dereddened Halpha luminosity is about 0.4 M_sun yr^-1, and the total supernova rate from the integrated, dereddened [FeII] luminosity is about 0.005 yr^-1 (assuming a distance of 3.36 Mpc). The azimuthally averaged [FeII]/Brgamma flux ratio is larger at the edges of the central, gas-deficient cavities (encompassing the super star clusters A and B) and in the galaxy outskirts. If we interpret this line ratio as the ratio between the average past star formation (as traced by supernovae) and on-going activity (represented by OB stars able to ionize the interstellar medium), it would then indicate that star formation has been quenched within the central cavities and lately triggered in a ring around them. The number of ionizing hydrogen and helium photons as computed from the integrated, dereddened Halpha and HeI luminosities suggests that the latest burst of star formation occurred about 4 Myr ago and produced new stars with a total mass of ~1.8 x 10^6 M_sun. [Abridged], Comment: accepted for publication in AJ
Published: 2011
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132. The SIMPLE survey: observations, reduction, and catalog

Author: Damen, M., Labbe, I., van Dokkum, P. G., Franx, M., Taylor, E. N., Brandt, W. N., Dickinson, M., Gawiser, E., Illingworth, G. D., Kriek, M., Marchesini, D., Muzzin, A., Papovich, C., and Rix, H. -W.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the Spitzer IRAC/MUSYC Public Legacy Survey in the Extended CDF-South (SIMPLE), which consists of deep IRAC observations covering the ~1,600 arcmin^2 area surrounding GOODS-S. The limiting magnitudes of the SIMPLE IRAC mosaics typically are 23.8, 23.6, 21.9, and 21.7, at 3.6 um, 4.5 um, 5.8 um, and 8.0 um, respectively (5-sigma total point source magnitudes in AB). The SIMPLE IRAC images are combined with the 10'x15' GOODS IRAC mosaics in the center. We give detailed descriptions of the observations, data reduction, and properties of the final images, as well as the detection and photometry methods used to build a catalog. Using published optical and near-infrared data from the Multiwavelength Survey by Yale-Chile (MUSYC), we construct an IRAC-selected catalog, containing photometry in UBVRIz'JHK, [3.6 um], [4.5 um], [5.8 um], and [8.0 um]. The catalog contains 43,782 sources with S/N > 5 at 3.6 um, 19,993 of which have 13-band photometry. We compare this catalog to the publicly available MUSYC and FIREWORKS catalogs and discuss the differences. Using a high signal-to-noise sub-sample of 3,391 sources with ([3.6] + [4.5])/2 < 21.2, we investigate the star formation rate history of massive galaxies out to z ~ 1.8. We find that at z ~ 1.8 at least 30% +/-7% of the most massive galaxies (Mstar > 10^11 Msol) are passively evolving, in agreement with earlier results from surveys covering less area., Comment: 24 pages, 21 figures
Published: 2010
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133. The LABOCA survey of the Extended Chandra Deep Field South: A photometric redshift survey of submillimetre galaxies

Author: Wardlow, J. L., Smail, Ian, Coppin, K. E. K., Alexander, D. M., Brandt, W. N., Danielson, A. L. R., Luo, B., Swinbank, A. M., Walter, F., Weiss, A., Xue, Y. Q., Zibetti, S., Bertoldi, F., Biggs, A. D., Chapman, S. C., Dannerbauer, H., Dunlop, J. S., Gawiser, E., Ivison, R. J., Knudsen, K. K., Kovacs, A., Lacey, C. G., Menten, K. M., Padilla, N., Rix, H. -W., and van der Werf, P. P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [abridged] We derive photometric redshifts from 17-band optical to mid-IR photometry of 74 robust counterparts to 68 of the 126 submillimetre galaxies (SMGs) selected at 870um by LABOCA observations in the ECDFS. The median photometric redshift of identified SMGs is z=2.2\pm0.1, the interquartile range is z=1.8-2.7 and we identify 10 (~15%) high-redshift (z>3) SMGs. We derive a simple redshift estimator for SMGs based on the 3.6 and 8um fluxes, which is accurate to Delta_z~0.4 for SMGs at z<4. A statistical analysis of sources around unidentified SMGs identifies a population of likely counterparts with a redshift distribution peaking at z=2.5\pm0.3, which likely comprises ~60% of the unidentified SMGs. This confirms that the bulk of the undetected SMGs are coeval with those detected in the radio/mid-IR. We conclude that ~15% of all the SMGs are below the flux limits of our survey and lie at z>3 and hence ~30% of all SMGs have z>3. We estimate that the full S_870um>4mJy SMG population has a median redshift of 2.5\pm0.6. In contrast to previous suggestions we find no significant correlation between S_870um and redshift. The median stellar mass of the SMGs derived from SED fitting is (9.2\pm0.9)x10^10Msun and the interquartile range is (4.7-14)x10^10Msun, although we caution that uncertainty in the star-formation histories results in a factor of ~5 uncertainty in these stellar masses. The median characteristic dust temperature of SMGs is 35.9\pm1.4K and the interquartile range is 28.5-43.3K. The infrared luminosity function shows that SMGs at z=2-3 typically have higher far-IR luminosities and luminosity density than those at z=1-2. This is mirrored in the evolution of the star-formation rate density (SFRD) for SMGs which peaks at z~2. The maximum contribution of bright SMGs to the global SFRD (~5% for SMGs with S_870um>4mJy; ~50% for SMGs with S_870um>1mJy) also occurs at z~2., Comment: Submitted for publication in MNRAS: 31 pages, 15 figures, 4 tables
Published: 2010
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134. Herschel/PACS far-infrared photometry of two z>4 quasars

Author: Leipski, C., Meisenheimer, K., Klaas, U., Walter, F., Nielbock, M., Krause, O., Dannerbauer, H., Bertoldi, F., Besel, M. -A., de Rosa, G., Fan, X., Haas, M., Hutsemekers, D., Jean, C., Lemke, D., Rix, H. -W., and Stickel, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel far-infrared (FIR) observations of two sub-mm bright quasars at high redshift: SDSS J1148+5251 (z=6.42) and BR 1202-0725 (z=4.69) obtained with the PACS instrument. Both objects are detected in the PACS photometric bands. The Herschel measurements provide additional data points that constrain the FIR spectral energy distributions (SEDs) of both sources, and they emphasise a broad range of dust temperatures in these objects. For lambda_rest ~< 20mu, the two SEDs are very similar to the average SEDs of quasars at low redshift. In the FIR, however, both quasars show excess emission compared to low-z QSO templates, most likely from cold dust powered by vigorous star formation in the QSO host galaxies. For SDSS J1148+5251 we detect another object at 160mu with a distance of ~10 arcseconds from the QSO. Although no physical connection between the quasar and this object can be shown with the available data, it could potentially confuse low-resolution measurements, thus resulting in an overestimate of the FIR luminosity of the z=6.42 quasar., Comment: 4 pages, 3 figures, accepted for publication in the A&A special issue on Herschel
Published: 2010
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135. Mapping far-IR emission from the central kiloparsec of NGC 1097

Author: Sandstrom, K., Krause, O., Linz, H., Schinnerer, E., Dumas, G., Meidt, S., Rix, H. -W., Sauvage, M., Walter, F., Kennicutt, R. C., Calzetti, D., Appleton, P., Armus, L., Beirão, P., Bolatto, A., Brandl, B., Crocker, A., Croxall, K., Dale, D., Draine, B. T., Engelbracht, C., de Paz, A. Gil, Gordon, K., Groves, B., Hao, C. -N., Helou, G., Hinz, J., Hunt, L., Johnson, B. D., Koda, J., Leroy, A., Murphy, E. J., Rahman, N., Roussel, H., Skibba, R., Smith, J. -D., Srinivasan, S., Vigroux, L., Warren, B. E., Wilson, C. D., Wolfire, M., and Zibetti, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using photometry of NGC 1097 from the Herschel PACS (Photodetector Array Camera and Spectrometer) instrument, we study the resolved properties of thermal dust continuum emission from a circumnuclear starburst ring with a radius ~ 900 pc. These observations are the first to resolve the structure of a circumnuclear ring at wavelengths that probe the peak (i.e. lambda ~ 100 micron) of the dust spectral energy distribution. The ring dominates the far-infrared (far-IR) emission from the galaxy - the high angular resolution of PACS allows us to isolate the ring's contribution and we find it is responsible for 75, 60 and 55% of the total flux of NGC 1097 at 70, 100 and 160 micron, respectively. We compare the far-IR structure of the ring to what is seen at other wavelengths and identify a sequence of far-IR bright knots that correspond to those seen in radio and mid-IR images. The mid- and far-IR band ratios in the ring vary by less than +/- 20% azimuthally, indicating modest variation in the radiation field heating the dust on ~ 600 pc scales. We explore various explanations for the azimuthal uniformity in the far-IR colors of the ring including a lack of well-defined age gradients in the young stellar cluster population, a dominant contribution to the far-IR emission from dust heated by older (> 10 Myr) stars and/or a quick smoothing of local enhancements in dust temperature due to the short orbital period of the ring. Finally, we improve previous limits on the far-IR flux from the inner ~ 600 pc of NGC 1097 by an order of magnitude, providing a better estimate of the total bolometric emission arising from the active galactic nucleus and its associated central starburst., Comment: Accepted for publication in the A&A Herschel Special Edition
Published: 2010
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136. Enhanced dust heating in the bulges of early-type spiral galaxies

Author: Engelbracht, C. W., Hunt, L. K., Skibba, R. A., Hinz, J. L., Calzetti, D., Gordon, K. D., Roussel, H., Crocker, A. F., Misselt, K. A., Bolatto, A. D., Kennicutt, R. C., Appleton, P. N., Armus, L., Beirão, P., Brandl, B. R., Croxall, K. V., Dale, D. A., Draine, B. T., Dumas, G., de Paz, A. Gil, Groves, B., Hao, C. -N., Johnson, B. D., Koda, J., Krause, O., Leroy, A. K., Meidt, S. E., Murphy, E. J., Rahman, N., Rix, H. -W., Sandstrom, K. M., Sauvage, M., Schinnerer, E., Smith, J. -D. T., Srinivasan, S., Vigroux, L., Walter, F., Warren, B. E., Wilson, C. D., Wolfire, M. G., and Zibetti, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Stellar density and bar strength should affect the temperatures of the cool (T ~ 20-30 K) dust component in the inner regions of galaxies, which implies that the ratio of temperatures in the circumnuclear regions to the disk should depend on Hubble type. We investigate the differences between cool dust temperatures in the central 3 kpc and disk of 13 nearby galaxies by fitting models to measurements between 70 and 500 microns. We attempt to quantify temperature trends in nearby disk galaxies, with archival data from Spitzer/MIPS and new observations with Herschel/SPIRE, which were acquired during the first phases of the Herschel observations for the KINGFISH (key insights in nearby galaxies: a far-infrared survey with Herschel) sample. We fit single-temperature modified blackbodies to far-infrared and submillimeter measurements of the central and disk regions of galaxies to determine the temperature of the component(s) emitting at those wavelengths. We present the ratio of central-region-to-disk-temperatures of the cool dust component of 13 nearby galaxies as a function of morphological type. We find a significant temperature gradient in the cool dust component in all galaxies, with a mean center-to-disk temperature ratio of 1.15 +/- 0.03. The cool dust temperatures in the central ~3 kpc of nearby galaxies are 23(+/-3)% hotter for morphological types earlier than Sc, and only 9(+/-3)% hotter for later types. The temperature ratio is also correlated with bar strength, with only strongly barred galaxies having a ratio over 1.2. The strong radiation field in the high stellar density of a galactic bulge tends to heat the cool dust component to higher temperatures, at least in early-type spirals with relatively large bulges, especially when paired with a strong bar., Comment: Accepted for publication on the A&A Herschel Special Issue
Published: 2010
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137. Far-Infrared Line Imaging of the Starburst Ring in NGC 1097 with the Herschel/PACS Spectrometer

Author: Beirao, P., Armus, L., Appleton, P. N., Smith, J. -D. T., Croxall, K. V., Murphy, E. J., Dale, D. A., Helou, G., Kennicutt, R. C., Calzetti, D., Bolatto, A. D., Brandl, B. R., Crocker, A. F., Draine, B. T., Dumas, G., Engelbracht, C. W., de Paz, A. Gil, Gordon, K. D., Groves, B., Hao, C. -N., Hinz, J. L., Hunt, L. K., Johnson, B. D., Koda, J., Krause, O., Leroy, A. K., Meidt, S. E., Richer, J., Rix, H. -W., Rahman, N., Roussel, H., Sandstrom, K. M., Sauvage, M., Schinnerer, E., Skibba, R. A., Srinivasan, S., Walter, F., Warren, B. E., Wilson, C. D., Wolfire, M. G., and Zibetti, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: NGC 1097 is a nearby SBb galaxy with a Seyfert nucleus and a bright starburst ring. We study the physical properties of the interstellar medium (ISM) in the ring using spatially resolved far-infrared spectral maps of the circumnuclear starburst ring of NGC 1097, obtained with the PACS spectrometer on board the Herschel Space Telescope. In particular, we map the important ISM cooling and diagnostic emission lines of [OI] 63 $\mu$m, [OIII] 88 $\mu$m, [NII] 122 $\mu$m, [CII] 158 $\mu$m and [NII] 205 $\mu$m. We observe that in the [OI] 63 $\mu$m, [OIII] 88 $\mu$m, and [NII] 122 $\mu$m line maps, the emission is enhanced in clumps along the NE part of the ring. We observe evidence of rapid rotation in the circumnuclear ring, with a rotation velocity of ~220$ km s$^{-1}$ (inclination uncorrected) measured in all lines. The [OI] 63 $\mu$m/[CII] 158 $\mu$m ratio varies smoothly throughout the central region, and is enhanced on the northeastern part of the ring, which may indicate a stronger radiation field. This enhancement coincides with peaks in the [OI] 63 $\mu$m and [OIII] 88 $\mu$m maps. Variations of the [NII] 122 $\mu$m/[NII] 205 $\mu$m ratio correspond to a range in the ionized gas density between 150 and 400 cm$^{-3}$., Comment: Accepted for publication on the A&A Herschel Special Issue
Published: 2010
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138. Barred disks in dense environments

Author: Marinova, I., Jogee, S., Heiderman, A., Barazza, F. D., Gray, M. E., Barden, M., Wolf, C., Peng, C. Y., Bacon, D., Balogh, M., Bell, E. F., Bohm, A., Caldwell, J. A. R., Haussler, B., Heymans, C., Jahnke, K., van Kampen, E., Koposov, S., Lane, K., McIntosh, D. H., Meisenheimer, K., Rix, H. -W., Sanchez, S. F., Taylor, A., Wisotzki, L., and Zheng, X.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We investigate the properties of bright (MV <= -18) barred and unbarred disks in the Abell 901/902 cluster system at z~0.165 with the STAGES HST ACS survey. To identify and characterize bars, we use ellipse-fitting. We use visual classification, a Sersic cut, and a color cut to select disk galaxies, and find that the latter two methods miss 31% and 51%, respectively of disk galaxies identified through visual classification. This underscores the importance of carefully selecting the disk sample in cluster environments. However, we find that the global optical bar fraction in the clusters is ~30% regardless of the method of disk selection. We study the relationship of the optical bar fraction to host galaxy properties, and find that the optical bar fraction depends strongly on the luminosity of the galaxy and whether it hosts a prominent bulge or is bulgeless. Within a given absolute magnitude bin, the optical bar fraction increases for galaxies with no significant bulge component. Within each morphological type bin, the optical bar fraction increases for brighter galaxies. We find no strong trend (variations larger than a factor of 1.3) for the optical bar fraction with local density within the cluster between the core and virial radius (R ~ 0.25 to 1.2 Mpc). We discuss the implications of our results for the evolution of bars and disks in dense environments., Comment: 7 pages, 2 figures; To appear in "Tumbling, twisting, and winding galaxies: Pattern speeds along the Hubble sequence", E. M. Corsini and V. P. Debattista (eds.), Memorie della Societa` Astronomica Italiana
Published: 2010

139. An Observational Estimate for the Mean Secular Evolution Rate in Spiral Galaxies

Author: Foyle, K., Rix, H. -W., and Zibetti, S.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have observationally quantified the effect of gravitational torques on stars in disk galaxies due to the stellar distribution itself and explored whether these torques are efficient at transporting angular momentum within a Hubble Time. We derive instantaneous torque maps for a sample of 24 spiral galaxies, based on stellar mass maps that were derived using the pixel-by-pixel mass-to-light estimator by Zibetti, Rix and Charlot. In conjunction with an estimate of the rotation velocity, the mass maps allow us to determine the torque-induced instantaneous angular momentum flow across different radii, resulting from the overall stellar distributions for each galaxy in the sample. By stacking the sample, which effectively replaces a time average by an ensemble average, we find that the torques due to the stellar disk act to transport angular momentum outward over much of the disk (within 3 disk scale lengths). The strength of the ensemble-averaged gravitational torques within one disk scale length have a timescale of ~ 4 Gyr for angular momentum redistribution. This study is the first to observationally determine the strength of torque-driven angular momentum flow of stars for a sample of spiral galaxies, providing an important empirical constraint on secular evolution. (abridged), Comment: 24 pages, 18 Figures A high resolution version of this paper can be found at http://www.mpia-hd.mpg.de/~foyle/papers/MN-09-1350-MJ.pdf
Published: 2009
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140. Observational constraints on the co-evolution of supermassive black holes and galaxies

Author: Zheng, X. Z., Bell, E. F., Somerville, R. S., Rix, H. -W., Jahnke, K., Fontanot, F., Rieke, G. H., Schiminovich, D., and Meisenheimer, K.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The star formation rate (SFR) and black hole accretion rate (BHAR) functions are measured to be proportional to each other at z < ~3. This close correspondence between SF and BHA would naturally yield a BH mass-galaxy mass correlation, whereas a BH mass-bulge mass correlation is observed. To explore this apparent contradiction we study the SF in spheroid-dominated galaxies between z=1 and the present day. We use 903 galaxies from the COMBO-17 survey with M* >2x10^10M_sun, ultraviolet and infrared-derived SFRs from Spitzer and GALEX, and morphologies from GEMS HST/ACS imaging. Using stacking techniques, we find that <25% of all SF occurs in spheroid-dominated galaxies (Sersic index n>2.5), while the BHAR that we would expect if the global scalings held is three times higher. This rules out the simplest picture of co-evolution, in which SF and BHA trace each other at all times. These results could be explained if SF and BHA occur in the same events, but offset in time, for example at different stages of a merger event. However, one would then expect to see the corresponding star formation activity in early-stage mergers, in conflict with observations. We conclude that the major episodes of SF and BHA occur in different events, with the bulk of SF happening in isolated disks and most BHA occurring in major mergers. The apparent global co-evolution results from the regulation of the BH growth by the potential well of the galactic spheroid, which includes a major contribution from disrupted disk stars., Comment: 14 pages, 5 figures, accepted for publication in ApJ
Published: 2009
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141. The LABOCA Survey of the Extended Chandra Deep Field South

Author: Weiss, A., Kovacs, A., Coppin, K., Greve, T. R., Walter, F., Smail, Ian, Dunlop, J. S., Knudsen, K. K., Alexander, D. M., Bertoldi, F., Brandt, W. N., Chapman, S. C., Cox, P., Dannerbauer, H., De Breuck, C., Gawiser, E., Ivison, R. J., Lutz, D., Menten, K. M., Koekemoer, A. M., Kreysa, E., Kurczynski, P., Rix, H. -W., Schinnerer, E., and van der Werf, P. P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a sensitive 870 micron survey of the Extended Chandra Deep Field South (ECDFS) using LABOCA on the APEX telescope. The LABOCA ECDFS Submillimetre Survey (LESS) covers the full 30' x 30' field size of the ECDFS and has a uniform noise level of 1.2 mJy/beam. LESS is thus the largest contiguous deep submillimetre survey undertaken to date. The noise properties of our map show clear evidence that we are beginning to be affected by confusion noise. We present a catalog of 126 SMGs detected with a significance level above 3.7 sigma. The ECDFS exhibits a deficit of bright SMGs relative to previously studied blank fields but not of normal star-forming galaxies that dominate the extragalactic background light (EBL). This is in line with the underdensities observed for optically defined high redshift source populations in the ECDFS (BzKs, DRGs,optically bright AGN and massive K-band selected galaxies). The differential source counts in the full field are well described by a power law with a slope of alpha=-3.2, comparable to the results from other fields. We show that the shape of the source counts is not uniform across the field. The integrated 870 micron flux densities of our source-count models account for >65% of the estimated EBL from COBE measurements. We have investigated the clustering of SMGs in the ECDFS by means of a two-point correlation function and find evidence for strong clustering on angular scales <1'. Assuming a power law dependence for the correlation function and a typical redshift distribution for the SMGs we derive a spatial correlation length of r_0=13+/-6 h^-1 Mpc., Comment: 25 pages, 13 figures. Accepted for publication in ApJ
Published: 2009
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142. NIR spectroscopy of SDSS J0303-0019: a low luminosity, high Eddington ratio quasar at z~6

Author: Kurk, J. D., Walter, F., Fan, X., Jiang, L., Jester, S., Rix, H. -W., and Riechers, D. A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present sensitive near--infrared VLT ISAAC spectroscopic observations of the z=6.08 quasar SDSS J030331.40-001912.9. This QSO is more than a magnitude fainter than other QSOs at z~6 for which NIR spectroscopy has been obtained to date and is therefore presumably more representative of the QSO population at the end of Cosmic Reionization. Combining rest--frame UV continuum luminosity with the width measurements of the Mg II and C IV lines, we derive a black hole mass of 2(+1.0/-0.5) x 10^8 solar masses, the lowest mass observed for z~6 QSOs to date, and derive an Eddington ratio of 1.6(+0.4/-0.6), amongst the highest value derived for QSOs at any redshift. The Spitzer 24 micron non--detection of this QSO does not leave space for a significant hot dust component in its optical/near--infrared SED, in common with one other faint QSO at z=6, but in contrast to more than twenty more z=6 QSOs and all known lower redshift QSOs with sufficiently deep multi-wavelength photometry. We conclude that we have found evidence for differences in the intrinsic properties of at least one z~6 QSO as compared to the lower--redshift population., Comment: Accepted by ApJ on July 1, 2009; 5 pages, 2 figures
Published: 2009
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143. Gaia Data Release 3:Analysis of the Gaia BP/RP spectra using the General Stellar Parameterizer from Photometry

Author: Andrae, R., Fouesneau, M., Sordo, R., Bailer-Jones, C. A. L., Dharmawardena, T.E., Rybizki, Jan, De Angeli, F., Lindstrøm, Hans Erik Peter, Marshall, Dan, Drimmel, R., Korn, A, Soubiran, C., Brouillet, Nathalie, Casamiquela, L., Rix, H.-W., Abreu, António, Alvarez, Marta, Bakke, Jesse, Bellas-Velidis, I., Bijaoui, A., Andrae, R., Fouesneau, M., Sordo, R., Bailer-Jones, C. A. L., Dharmawardena, T.E., Rybizki, Jan, De Angeli, F., Lindstrøm, Hans Erik Peter, Marshall, Dan, Drimmel, R., Korn, A, Soubiran, C., Brouillet, Nathalie, Casamiquela, L., Rix, H.-W., Abreu, António, Alvarez, Marta, Bakke, Jesse, Bellas-Velidis, I., and Bijaoui, A.
Published: 2023

144. Euclid preparation – XXIII. Derivation of galaxy physical properties with deep machine learning using mock fluxes and H-band images

Author: Collaboration, Euclid, Bisigello, L, Conselice, C J, Baes, M, Bolzonella, M, Brescia, M, Cavuoti, S, Cucciati, O, Humphrey, A, Hunt, L K, Maraston, C, Pozzetti, L, Tortora, C, van Mierlo, S E, Aghanim, N, Auricchio, N, Baldi, M, Bender, R, Bodendorf, C, Bonino, D, Branchini, E, Brinchmann, J, Camera, S, Capobianco, V, Carbone, C, Carretero, J, Castander, F J, Castellano, M, Cimatti, A, Congedo, G, Conversi, L, Copin, Y, Corcione, L, Courbin, F, Cropper, M, Da Silva, A, Degaudenzi, H, Douspis, M, Dubath, F, Duncan, C A J, Dupac, X, Dusini, S, Farrens, S, Ferriol, S, Frailis, M, Franceschi, E, Franzetti, P, Fumana, M, Garilli, B, Gillard, W, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Guzzo, L, Haugan, S V H, Holmes, W, Hormuth, F, Hornstrup, A, Jahnke, K, Kümmel, M, Kermiche, S, Kiessling, A, Kilbinger, M, Kohley, R, Kunz, M, Kurki-Suonio, H, Ligori, S, Lilje, P B, Lloro, I, Maiorano, E, Mansutti, O, Marggraf, O, Markovic, K, Marulli, F, Massey, R, Maurogordato, S, Medinaceli, E, Meneghetti, M, Merlin, E, Meylan, G, Moresco, M, Moscardini, L, Munari, E, Niemi, S M, Padilla, C, Paltani, S, Pasian, F, Pedersen, K, Pettorino, V, Polenta, G, Poncet, M, Popa, L, Raison, F, Renzi, A, Rhodes, J, Riccio, G, Rix, H -W, Romelli, E, Roncarelli, M, Rosset, C, Rossetti, E, Saglia, R, Sapone, D, Sartoris, B, Schneider, P, Scodeggio, M, Secroun, A, Seidel, G, Sirignano, C, Sirri, G, Stanco, L, Tallada-Crespí, P, Tavagnacco, D, Taylor, A N, Tereno, I, Toledo-Moreo, R, Torradeflot, F, Tutusaus, I, Valentijn, E A, Valenziano, L, Vassallo, T, Wang, Y, Zacchei, A, Zamorani, G, Zoubian, J, Andreon, S, Bardelli, S, Boucaud, A, Colodro-Conde, C, Ferdinando, D Di, Graciá-Carpio, J, Lindholm, V, Maino, D, Mei, S, Scottez, V, Sureau, F, Tenti, M, Zucca, E, Borlaff, A S, Ballardini, M, Biviano, A, Bozzo, E, Burigana, C, Cabanac, R, Cappi, A, Carvalho, C S, Casas, S, Castignani, G, Cooray, A, Coupon, J, Courtois, H M, Cuby, J, Davini, S, De Lucia, G, Desprez, G, Dole, H, Escartin, J A, Escoffier, S, Farina, M, Fotopoulou, S, Ganga, K, Garcia-Bellido, J, George, K, Giacomini, F, Gozaliasl, G, Hildebrandt, H, Hook, I, Huertas-Company, M, Kansal, V, Keihanen, E, Kirkpatrick, C C, Loureiro, A, Macías-Pérez, J F, Magliocchetti, M, Mainetti, G, Marcin, S, Martinelli, M, Martinet, N, Metcalf, R B, Monaco, P, Morgante, G, Nadathur, S, Nucita, A A, Patrizii, L, Peel, A, Potter, D, Pourtsidou, A, Pöntinen, M, Reimberg, P, Sánchez, A G, Sakr, Z, Schirmer, M, Sefusatti, E, Sereno, M, Stadel, J, Teyssier, R, Valieri, C, Valiviita, J, Viel, M, Collaboration, Euclid, Bisigello, L, Conselice, C J, Baes, M, Bolzonella, M, Brescia, M, Cavuoti, S, Cucciati, O, Humphrey, A, Hunt, L K, Maraston, C, Pozzetti, L, Tortora, C, van Mierlo, S E, Aghanim, N, Auricchio, N, Baldi, M, Bender, R, Bodendorf, C, Bonino, D, Branchini, E, Brinchmann, J, Camera, S, Capobianco, V, Carbone, C, Carretero, J, Castander, F J, Castellano, M, Cimatti, A, Congedo, G, Conversi, L, Copin, Y, Corcione, L, Courbin, F, Cropper, M, Da Silva, A, Degaudenzi, H, Douspis, M, Dubath, F, Duncan, C A J, Dupac, X, Dusini, S, Farrens, S, Ferriol, S, Frailis, M, Franceschi, E, Franzetti, P, Fumana, M, Garilli, B, Gillard, W, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Guzzo, L, Haugan, S V H, Holmes, W, Hormuth, F, Hornstrup, A, Jahnke, K, Kümmel, M, Kermiche, S, Kiessling, A, Kilbinger, M, Kohley, R, Kunz, M, Kurki-Suonio, H, Ligori, S, Lilje, P B, Lloro, I, Maiorano, E, Mansutti, O, Marggraf, O, Markovic, K, Marulli, F, Massey, R, Maurogordato, S, Medinaceli, E, Meneghetti, M, Merlin, E, Meylan, G, Moresco, M, Moscardini, L, Munari, E, Niemi, S M, Padilla, C, Paltani, S, Pasian, F, Pedersen, K, Pettorino, V, Polenta, G, Poncet, M, Popa, L, Raison, F, Renzi, A, Rhodes, J, Riccio, G, Rix, H -W, Romelli, E, Roncarelli, M, Rosset, C, Rossetti, E, Saglia, R, Sapone, D, Sartoris, B, Schneider, P, Scodeggio, M, Secroun, A, Seidel, G, Sirignano, C, Sirri, G, Stanco, L, Tallada-Crespí, P, Tavagnacco, D, Taylor, A N, Tereno, I, Toledo-Moreo, R, Torradeflot, F, Tutusaus, I, Valentijn, E A, Valenziano, L, Vassallo, T, Wang, Y, Zacchei, A, Zamorani, G, Zoubian, J, Andreon, S, Bardelli, S, Boucaud, A, Colodro-Conde, C, Ferdinando, D Di, Graciá-Carpio, J, Lindholm, V, Maino, D, Mei, S, Scottez, V, Sureau, F, Tenti, M, Zucca, E, Borlaff, A S, Ballardini, M, Biviano, A, Bozzo, E, Burigana, C, Cabanac, R, Cappi, A, Carvalho, C S, Casas, S, Castignani, G, Cooray, A, Coupon, J, Courtois, H M, Cuby, J, Davini, S, De Lucia, G, Desprez, G, Dole, H, Escartin, J A, Escoffier, S, Farina, M, Fotopoulou, S, Ganga, K, Garcia-Bellido, J, George, K, Giacomini, F, Gozaliasl, G, Hildebrandt, H, Hook, I, Huertas-Company, M, Kansal, V, Keihanen, E, Kirkpatrick, C C, Loureiro, A, Macías-Pérez, J F, Magliocchetti, M, Mainetti, G, Marcin, S, Martinelli, M, Martinet, N, Metcalf, R B, Monaco, P, Morgante, G, Nadathur, S, Nucita, A A, Patrizii, L, Peel, A, Potter, D, Pourtsidou, A, Pöntinen, M, Reimberg, P, Sánchez, A G, Sakr, Z, Schirmer, M, Sefusatti, E, Sereno, M, Stadel, J, Teyssier, R, Valieri, C, Valiviita, J, and Viel, M
Abstract: Next-generation telescopes, like Euclid, Rubin/LSST, and Roman, will open new windows on the Universe, allowing us to infer physical properties for tens of millions of galaxies. Machine-learning methods are increasingly becoming the most efficient tools to handle this enormous amount of data, because they are often faster and more accurate than traditional methods. We investigate how well redshifts, stellar masses, and star-formation rates (SFRs) can be measured with deep-learning algorithms for observed galaxies within data mimicking the Euclid and Rubin/LSST surveys. We find that deep-learning neural networks and convolutional neural networks (CNNs), which are dependent on the parameter space of the training sample, perform well in measuring the properties of these galaxies and have a better accuracy than methods based on spectral energy distribution fitting. CNNs allow the processing of multiband magnitudes together with HE-band images. We find that the estimates of stellar masses improve with the use of an image, but those of redshift and SFR do not. Our best results are deriving (i) the redshift within a normalized error of <0.15 for 99.9 per cent of the galaxies with signal-to-noise ratio >3 in the HE band; (ii) the stellar mass within a factor of two (⁠∼0.3 dex⁠) for 99.5 per cent of the considered galaxies; and (iii) the SFR within a factor of two (⁠∼0.3 dex⁠) for ∼70 per cent of the sample. We discuss the implications of our work for application to surveys as well as how measurements of these galaxy parameters can be improved with deep learning.
Published: 2023

145. Identification and properties of intense star-forming galaxies at redshifts z > 10

Author: Robertson, B. E., Tacchella, S., Johnson, B. D., Hainline, K., Whitler, L., Eisenstein, D. J., Endsley, R., Rieke, M., Stark, D. P., Alberts, S., Dressler, A., Egami, E., Hausen, R., Rieke, G., Shivaei, I., Williams, C. C., Willmer, C. N. A., Arribas, S., Bonaventura, N., Bunker, A., Cameron, A. J., Carniani, S., Charlot, S., Chevallard, J., Curti, M., Curtis-Lake, E., D'Eugenio, F., Jakobsen, P., Looser, T. J., Lutzgendorf, N., Maiolino, R., Maseda, M. V., Rawle, T., Rix, H. -W., Smit, R., Ubler, H., Willott, C., Witstok, J., Baum, S., Bhatawdekar, R., Boyett, K., Chen, Z., de Graaff, A., Florian, M., Helton, J. M., Hviding, R. E., Ji, Z., Kumari, N., Lyu, J., Nelson, E., Sandles, L., Saxena, A., Suess, K. A., Sun, F., Topping, M., Wallace, I. E. B., Robertson, B. E., Tacchella, S., Johnson, B. D., Hainline, K., Whitler, L., Eisenstein, D. J., Endsley, R., Rieke, M., Stark, D. P., Alberts, S., Dressler, A., Egami, E., Hausen, R., Rieke, G., Shivaei, I., Williams, C. C., Willmer, C. N. A., Arribas, S., Bonaventura, N., Bunker, A., Cameron, A. J., Carniani, S., Charlot, S., Chevallard, J., Curti, M., Curtis-Lake, E., D'Eugenio, F., Jakobsen, P., Looser, T. J., Lutzgendorf, N., Maiolino, R., Maseda, M. V., Rawle, T., Rix, H. -W., Smit, R., Ubler, H., Willott, C., Witstok, J., Baum, S., Bhatawdekar, R., Boyett, K., Chen, Z., de Graaff, A., Florian, M., Helton, J. M., Hviding, R. E., Ji, Z., Kumari, N., Lyu, J., Nelson, E., Sandles, L., Saxena, A., Suess, K. A., Sun, F., Topping, M., and Wallace, I. E. B.
Abstract: Surveys with the James Webb Space Telescope (JWST) have discovered candidate galaxies in the first 400 Myr of cosmic time. Preliminary indications have suggested these candidate galaxies may be more massive and abundant than previously thought. However, without confirmed distances, their inferred properties remain uncertain. Here we identify four galaxies located in the JWST Advanced Deep Extragalactic Survey Near-Infrared Camera imaging with photometric redshifts z of roughly 10-13. These galaxies include the first redshift z > 12 systems discovered with distances spectroscopically confirmed by JWST in a companion paper. Using stellar population modelling, we find the galaxies typically contain 100 million solar masses in stars, in stellar populations that are less than 100 million years old. The moderate star-formation rates and compact sizes suggest elevated star-formation rate surface densities, a key indicator of their formation pathways. Taken together, these measurements show that the first galaxies contributing to cosmic reionization formed rapidly and with intense internal radiation fields.The JWST Advanced Deep Extragalactic Survey using NIRCam to find the earliest galaxies reveals the size and star formation rates of four extreme redshift (z > 10) galaxies of the distant Universe.
Published: 2023

146. Barred Galaxies in the Abell 901/2 Supercluster with STAGES

Author: Marinova, I., Jogee, S., Heiderman, A., Barazza, F. D., Gray, M. E., Barden, M., Wolf, C., Peng, C. Y., Bacon, D., Balogh, M., Bell, E. F., Bohm, A., Caldwell, J. A. R., Haussler, B., Heymans, C., Jahnke, K., van Kampen, E., Koposov, S., Lane, K., McIntosh, D. H., Meisenheimer, K., Rix, H. -W., Sanchez, S. F., Taylor, A., Wisotzki, L., and Zheng, X.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present a study of bar and host disk evolution in a dense cluster environment, based on a sample of ~800 bright (MV <= -18) galaxies in the Abell 901/2 supercluster at z~0.165. We use HST ACS F606W imaging from the STAGES survey, and data from Spitzer, XMM-Newton, and COMBO-17. We identify and characterize bars through ellipse-fitting, and other morphological features through visual classification. (1) We explore three commonly used methods for selecting disk galaxies. We find 625, 485, and 353 disk galaxies, respectively, via visual classification, a single component S'ersic cut (n <= 2.5), and a blue-cloud cut. In cluster environments, the latter two methods miss 31% and 51%, respectively, of visually-identified disks. (2) For moderately inclined disks, the three methods of disk selection yield a similar global optical bar fraction (f_bar-opt) of 34% +10%/-3%, 31% +10%/-3%, and 30% +10%/-3%, respectively. (3) f_bar-opt rises in brighter galaxies and those which appear to have no significant bulge component. Within a given absolute magnitude bin, f_bar-opt is higher in visually-selected disk galaxies that have no bulge as opposed to those with bulges. For a given morphological class, f_bar-opt rises at higher luminosities. (4) For bright early-types, as well as faint late-type systems with no evident bulge, the optical bar fraction in the Abell 901/2 clusters is comparable within a factor of 1.1 to 1.4 to that of field galaxies at lower redshifts (5) Between the core and the virial radius of the cluster at intermediate environmental densities, the optical bar fraction does not appear to depend strongly on the local environment density and varies at most by a factor of ~1.3. We discuss the implications of our results for the evolution of bars and disks in dense environments., Comment: accepted for publication in ApJ, abstract abridged, for high resolution figures see http://www.as.utexas.edu/~marinova/STAGES/STAGES_bars.pdf
Published: 2009
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147. Halo streams in the 7th SDSS data release

Author: Klement, R., Rix, H. -W., Flynn, C., Fuchs, B., Beers, T. C., Prieto, C. Allende, Bizyaev, D., Brewington, H., Lee, Y. S., Malanushenko, E., Malanushenko, V., Oravetz, D., Pan, K., Fiorentin, P. Re, Simmons, A., and Snedden, S.
Subjects: Astrophysics - Galaxy Astrophysics
Abstract: We have detected stellar halo streams in the solar neighborhood using data from the 7th public data release of the Sloan Digital Sky Survey (SDSS), which includes the directed stellar program SEGUE: Sloan Extension For Galactic Understanding and Exploration. In order to derive distances to each star, we used the metallicity-dependent photometric parallax relation from Ivezic et al. (2008) for which we examine and quantify the accuracy. Our final sample consists of 22,321 nearby (d < 2 kpc), metal-poor ([Fe/H] < -0.5) main-sequence stars with 6D estimates of position and space velocity. We characterize the orbits of these stars through suitable kinematic proxies for their "effective" integrals of motion, angular momentum, eccentricity, and orbital polar angle and compare the observed distribution to expectations from a smooth distribution in four [Fe/H] bins. On this basis we identify at least five significant "phase-space overdensities" of stars on very similar orbits in the solar neighborhood to which we can assign unambiguously peaked [Fe/H] distributions. Three of them have been identified previously, including the halo stream discovered by Helmi et al. (1999) at a significance level of 12.0. In addition, we find at least two new genuine halo streams, judged by their kinematics and [Fe/H], at significance levels of 2.9 and 4.8, respectively. For one stream the stars even show coherence in configuration space, matching a spatial overdensity of stars found by Juric et al. (2008) at (R,z) \approx (9.5,0.8) kpc. Our results demonstrate the practical power of our search method to detect substructure in the phase-space distribution of nearby stars without making a-priori assumptions about the detailed form of the gravitational potential., Comment: 57 pages, 22 figures, accepted for publication in ApJ
Published: 2009
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148. A LABOCA survey of the Extended Chandra Deep Field South - submillimeter properties of near-IR selected galaxies

Author: Greve, T. R., Weiss, A., Walter, F., Smail, I., Zheng, X. Z., Knudsen, K. K., Coppin, K. E. K., Kovacs, A., Bell, E. F., de Breuck, C., Dannerbauer, H., Dickinson, M., Gawiser, E., Lutz, D., Rix, H. -W., Schinnerer, E., Alexander, D., Bertoldi, F., Brandt, W. N., Chapman, S. C., Ivison, R. J., Koekemoer, A. M., Kreysa, E., Kurczynski, P., Menten, K., Siringo, G., Swinbank, M., and van der Werf, P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using the 330hr ESO-MPG 870-micron survey of the Extended Chandra Deep Field South (ECDF-S) obtained with the Large Apex BOlometer CAmera (LABOCA) on the Atacama Pathfinder EXperiment (APEX), we have carried out a stacking analysis at submillimeter (submm) wavelengths of a sample of 8266 near-infra-red (near-IR) selected (K_vega <= 20) galaxies, including 893 BzK galaxies, 1253 extremely red objects (EROs) and 737 distant red galaxies (DRGs), selected from the Multi-wavelength Survey by Yale-Chile (MUSYC). We measure average 870-micron fluxes of 0.20+-0.01mJy (20.0sigma), 0.45+-0.04mJy (11.3sigma), 0.42+-0.03mJy (14.0sigma), and 0.41+-0.04mJy (10.3sigma) for the K_vega <= 20, BzK, ERO and DRG samples, respectively. For the BzK, ERO and DRG subsamples, which overlap to some degree and are like to be at z ~ 1-2, this implies an average far-IR luminosity of ~2-6x10^{11} Lsolar and star formation rate of ~40-100Msolar. Splitting the BzK galaxies up into star-forming (sBzK) and passive (pBzK) galaxies, the former is significantly detected (0.48+-0.04mJy, 12.0sigma) while the latter is only marginally detected (0.27+-0.10mJy, 2.7sigma), thus confirming that the sBzK/pBzK criteria do isolate obscured, star forming and truly passive galaxies. The K_vega <= 20 galaxies are found to contribute with 6.6+-0.3Jy deg^{-2} (~15%) to the 870-micron extragalactic background light (EBL). sBzK and pBzK galaxies contribute 1.7+-0.2Jy deg^{-2} (~4%) and 0.2+-0.1 Jy deg^{-2} (< 0.5%) to the EBL. [Abridged], Comment: (21 pages, 11 figures, submitted to ApJ)
Published: 2009
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149. What is Driving the HI Velocity Dispersion?

Author: Tamburro, D., Rix, H. -W., Leroy, A. K., Mac Low, M. -M., Walter, F., Kennicutt, R. C., Brinks, E., and de Blok, W. J. G.
Subjects: Astrophysics - Galaxy Astrophysics
Abstract: We explore what dominant physical mechanism sets the kinetic energy contained in neutral, atomic (HI) gas. We compare the HI line widths predicted from turbulence driven by supernova (SN) explosions and magneto-rotational instability (MRI) to direct observations in 11 disk galaxies. We use high-quality maps of the HI mass surface density and line width, obtained by the THINGS survey. We show that all sample galaxies exhibit a systematic radial decline in the HI line width, which appears to be a generic property of HI disks and also implies a radial decline in kinetic energy density of HI. At a galactocentric radius of r25 there is a characteristic value of the HI velocity dispersion of $10\pm2$ \kms. Inside this radius, galaxies show HI line widths above the thermal value expected from a warm HI component, implying that turbulence drivers must be responsible for maintaining this line width. Therefore, we compare maps of HI kinetic energy to maps of the star formation rate (SFR) and to predictions for energy generated by MRI. We find a positive correlation between kinetic energy of HI and SFR. For a given turbulence dissipation timescale we can estimate the energy input required to maintain the observed kinetic energy. The SN rate implied by the observed recent SFR is sufficient to maintain the observed velocity dispersion, if the SN feedback efficiency is at least \epsilon_SN\simeq0.1. Beyond r25, this efficiency would have to increase to unrealistic values, $\epsilon>1$, suggesting that mechanical energy from young stars does not supply most energy in outer disks. On the other hand, both thermal broadening and turbulence driven by MRI can produce the velocity dispersions and kinetic energies that we observe in this regime.
Published: 2009
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150. The kinematics of late type stars in the solar cylinder studied with SDSS data

Author: Fuchs, B., Dettbarn, C., Rix, H. -W., Beers, T. C., Bizyaev, D., Brewington, H., Jahreiss, H., Klement, R., Malanushenko, E., Malanushenko, V., Oravetz, D., Pan, K., Simmons, A., and Snedden, S.
Subjects: Astrophysics - Galaxy Astrophysics
Abstract: We study the velocity distribution of Milky Way disk stars in a kiloparsec-sized region around the Sun, based on ~ 2 million M-type stars from DR7 of SDSS, which have newly re-calibrated absolute proper motions from combining SDSS positions with the USNO-B catalogue. We estimate photometric distances to all stars, accurate to ~ 20 %, and combine them with the proper motions to derive tangential velocities for this kinematically unbiased sample of stars. Based on a statistical de-projection method we then derive the vertical profiles (to heights of Z = 800 pc above the disk plane) for the first and second moments of the three dimensional stellar velocity distribution. We find that = -7 +/- 1 km/s and = -9 +/- 1 km/s, independent of height above the mid-plane, reflecting the Sun's motion with respect to the local standard of rest. In contrast, changes distinctly from -20 +/- 2 km/s in the mid-plane to = -32 km/s at Z = 800 pc, reflecting an asymmetric drift of the stellar mean velocity that increases with height. All three components of the M-star velocity dispersion show a strong linear rise away from the mid-plane, most notably \sigma_{ZZ}, which grows from 18 km/s (Z = 0) to 40 km/s (at Z = 800 pc). We determine the orientation of the velocity ellipsoid, and find a significant vertex deviation of 20 to 25 degrees, which decreases only slightly to heights of Z = 800 pc. Away from the mid-plane, our sample exhibits a remarkably large tilt of the velocity ellipsoid towards the Galactic plane, which reaches 20 deg. at Z = 800 pc and which is not easily explained. Finally, we determine the ratio \sigma^2_{\phi\phi}/\sigma^2_{RR} near the mid-plane, which in the epicyclic approximation implies an almost perfectly flat rotation curve at the Solar radius., Comment: 18 pages, 9 figures, accepted to Astron. J
Published: 2009
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