Author: "Zamojski, M." - Searchworks@Jio Institute Digital Library Search Results

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115 results on '"Zamojski, M."'

1. Molecular gas properties of a lensed star-forming galaxy at z~3.6: a case study

Author: Dessauges-Zavadsky, M., Zamojski, M., Rujopakarn, W., Richard, J., Sklias, P., Schaerer, D., Combes, F., Ebeling, H., Rawle, T. D., Egami, E., Boone, F., Clément, B., Kneib, J. -P., Nyland, K., and Walth, G.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report on the galaxy MACSJ0032-arc at z=3.6314 discovered during the Herschel Lensing snapshot Survey of massive galaxy clusters, and strongly lensed by the cluster MACSJ0032.1+1808. The successful detections of its rest-frame UV, optical, FIR, millimeter, and radio continua, and of its CO emission enable us to characterize, for the first time at such a high redshift, the stellar, dust, and molecular gas properties of a compact star-forming galaxy with a size smaller than 2.5 kpc, a fairly low stellar mass of 4.8x10^9 Msun, and a moderate IR luminosity of 4.8x10^11 Lsun. We find that the bulk of the molecular gas mass and star formation seems to be spatially decoupled from the rest-frame UV emission. About 90% of the total star formation rate is undetected at rest-frame UV wavelengths because of severe obscuration by dust, but is seen through the thermal FIR dust emission and the radio synchrotron radiation. The observed CO(4-3) and CO(6-5) lines demonstrate that high-J transitions, at least up to J=6, remain excited in this galaxy, whose CO spectral line energy distribution resembles that of high-redshift submm galaxies, even though the IR luminosity of MACSJ0032-arc is ten times lower. This high CO excitation is possibly due to the compactness of the galaxy. We find evidence that this high CO excitation has to be considered in the balance when estimating the CO-to-H2 conversion factor. The inferred depletion time of the molecular gas in MACSJ0032-arc supports the decrease in the gas depletion timescale of galaxies with redshift, although to a lesser degree than predicted by galaxy evolution models. Instead, the measured molecular gas fraction as high as 60-79% in MACSJ0032-arc favors the continued increase in the gas fraction of galaxies with redshift as expected, despite the plateau observed between z~1.5 and z~2.5., Comment: 18 pages, 11 figures, 2 tables. Revised version accepted for publication in A&A
Published: 2016
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2. Nonstandard Errors

Author: MENKVELD, AJ, DREBER, A, HOLZMEISTER, F, HUBER, J, JOHANNESSON, M, KIRCHLER, M, NEUSÜß, S, RAZEN, M, WEITZEL, U, ABAD‐DÍAZ, D, ABUDY, M, MANO, N, MARCHAL, A, MARTINEAU, C, MAZZOLA, F, MELOSO, D, MI, MG, MIHET, R, MOHAN, V, MOINAS, S, ANGEL, JJ, GEMAYEL, R, MOORE, D, MU, L, MURAVYEV, D, MURPHY, D, NESZVEDA, G, NEUMEIER, C, NIELSSON, U, NIMALENDRAN, M, NOLTE, S, NORDEN, LL, GERRITSEN, D, AVETIKIAN, AT, O'NEILL, P, OBAID, K, ØDEGAARD, BA, ÖSTBERG, P, PAGNOTTA, E, PAINTER, M, PALAN, S, PALIT, IJ, PARK, A, GIL‐BAZO, J, PASCUAL, R, BACH, A, PASQUARIELLO, P, PASTOR, L, PATEL, V, PATTON, AJ, PEARSON, ND, PELIZZON, L, PELLI, M, PELSTER, M, GILDER, D, PÉRIGNON, C, PFIFFER, C, BAIDOO, E, PHILIP, R, PLÍHAL, T, PRAKASH, P, PRESS, O, PRODROMOU, T, PROKOPCZUK, M, PUTNINS, T, GLOSTEN, LR, QIAN, Y, RAIZADA, G, RAKOWSKI, D, BAKALLI, G, RANALDO, A, REGIS, L, REITZ, S, RENAULT, T, RENJIE, RW, RENO, R, GOMEZ, T, RIDDIOUGH, SJ, RINNE, K, RINTAMÄKI, P, RIORDAN, R, BAO, L, RITTMANNSBERGER, T, LONGARELA, IR, ROESCH, D, ROGNONE, L, ROSEMAN, B, GORBENKO, A, ROŞU, I, ROY, S, RUDOLF, N, RUSH, SR, RZAYEV, K, BARBON, A, RZEŹNIK, AA, SANFORD, A, SANKARAN, H, SARKAR, A, GRAMMIG, J, SARNO, L, SCAILLET, O, SCHARNOWSKI, S, SCHENK‐HOPPÉ, KR, SCHERTLER, A, SCHNEIDER, M, BASHCHENKO, O, SCHROEDER, F, SCHÜRHOFF, N, SCHUSTER, P, GRÉGOIRE, V, SCHWARZ, MA, SEASHOLES, MS, SEEGER, NJ, SHACHAR, O, SHKILKO, A, SHUI, J, SIKIC, M, BINDRA, PC, SIMION, G, SMALES, LA, GÜÇBILMEZ, U, SÖDERLIND, P, SOJLI, E, SOKOLOV, K, SÖNKSEN, J, SPOKEVICIUTE, L, STEFANOVA, D, SUBRAHMANYAM, MG, SZASZI, B, BJØNNES, GH, TALAVERA, O, ADRIAN, T, TANG, Y, TAYLOR, N, THAM, W, THEISSEN, E, THIMME, J, TONKS, I, TRAN, H, TRAPIN, L, TROLLE, AB, BLACK, JR, HAGSTRÖMER, B, VADUVA, MA, VALENTE, G, VAN NESS, RA, VASQUEZ, A, VEROUSIS, T, VERWIJMEREN, P, VILHELMSSON, A, VILKOV, G, VLADIMIROV, V, VOGEL, S, HAMBUCKERS, J, BLACK, BS, VOIGT, S, WAGNER, W, WALTHER, T, WEISS, P, VAN DER WEL, M, WERNER, IM, WESTERHOLM, PJ, WESTHEIDE, C, WIKA, HC, HAPNES, E, WIPPLINGER, E, BOGOEV, D, WOLF, M, WOLFF, CCP, WOLK, L, WONG, W, WRAMPELMEYER, J, WU, Z, XIA, S, XIU, D, HARRIS, JH, XU, K, XU, C, CORREA, SB, YADAV, PK, YAGÜE, J, YAN, C, YANG, A, YOO, W, YU, W, YU, Y, HARRIS, L, YU, S, YUESHEN, BZ, YUFEROVA, D, BONDARENKO, O, ZAMOJSKI, M, ZAREEI, A, ZEISBERGER, SM, ZHANG, L, ZHANG, SS, ZHANG, X, HARTMANN, S, ZHAO, L, ZHONG, Z, ZHOU, ZI, ZHOU, C, BOS, CS, ZHU, XS, ZOICAN, M, ZWINKELS, R, BOSCH‐ROSA, C, BOURI, E, HASSE, J, BROWNLEES, C, CALAMIA, A, CAO, VN, CAPELLE‐BLANCARD, G, ROMERO, LMC, CAPORIN, M, CARRION, A, CASKURLU, T, CHAKRABARTY, B, CHEN, J, HAUTSCH, N, CHERNOV, M, CHEUNG, W, CHINCARINI, LB, CHORDIA, T, CHOW, S, CLAPHAM, B, COLLIARD, J, COMERTON‐FORDE, C, CURRAN, E, DAO, T, HE, X, DARE, W, DAVIES, RJ, DE BLASIS, R, DE NARD, GF, DECLERCK, F, DEEV, O, DEGRYSE, H, DEKU, SY, DESAGRE, C, VAN DIJK, MA, HEATH, D, DIM, C, DIMPFL, T, DONG, YJ, DRUMMOND, PA, DUDDA, T, DUEVSKI, T, DUMITRESCU, A, DYAKOV, T, DYHRBERG, AH, DZIELIŃSKI, M, AIT‐SAHALIA, Y, EKSI, A, KALAK, IE, ELLEN, ST, EUGSTER, N, EVANS, MDD, FARRELL, M, FELEZ‐VINAS, E, FERRARA, G, FERROUHI, EM, FLORI, A, HEDIGER, S, FLUHARTY‐JAIDEE, JT, FOLEY, SDV, FONG, KYL, FOUCAULT, T, FRANUS, T, FRANZONI, F, FRIJNS, B, FRÖMMEL, M, FU, SM, FÜLLBRUNN, SC, HENDERSHOTT, T, GAN, B, GAO, G, GEHRIG, TP, HIBBERT, AM, HJALMARSSON, E, HOELSCHER, SA, HOFFMANN, P, HOLDEN, CW, HORENSTEIN, AR, HUANG, W, HUANG, D, AKMANSOY, O, HURLIN, C, ILCZUK, K, IVASHCHENKO, A, IYER, SR, JAHANSHAHLOO, H, JALKH, N, JONES, CM, JURKATIS, S, JYLHÄ, P, KAECK, AT, ALCOCK, JT, KAISER, G, KARAM, A, KARMAZIENE, E, KASSNER, B, KAUSTIA, M, KAZAK, E, KEARNEY, F, VAN KERVEL, V, KHAN, SA, KHOMYN, MK, ALEXEEV, V, KLEIN, T, KLEIN, O, KLOS, A, KOETTER, M, KOLOKOLOV, A, KORAJCZYK, RA, KOZHAN, R, KRAHNEN, JP, KUHLE, P, KWAN, A, ALOOSH, A, LAJAUNIE, Q, LAM, FYEC, LAMBERT, M, LANGLOIS, H, LAUSEN, J, LAUTER, T, LEIPPOLD, M, LEVIN, V, LI, Y, LI, H, AMATO, L, LIEW, CY, LINDNER, T, LINTON, O, LIU, J, LIU, A, LLORENTE, G, LOF, M, LOHR, A, LONGSTAFF, F, LOPEZ‐LIRA, A, AMAYA, D, MANKAD, S, MENKVELD, AJ, DREBER, A, HOLZMEISTER, F, HUBER, J, JOHANNESSON, M, KIRCHLER, M, NEUSÜß, S, RAZEN, M, WEITZEL, U, ABAD‐DÍAZ, D, ABUDY, M, MANO, N, MARCHAL, A, MARTINEAU, C, MAZZOLA, F, MELOSO, D, MI, MG, MIHET, R, MOHAN, V, MOINAS, S, ANGEL, JJ, GEMAYEL, R, MOORE, D, MU, L, MURAVYEV, D, MURPHY, D, NESZVEDA, G, NEUMEIER, C, NIELSSON, U, NIMALENDRAN, M, NOLTE, S, NORDEN, LL, GERRITSEN, D, AVETIKIAN, AT, O'NEILL, P, OBAID, K, ØDEGAARD, BA, ÖSTBERG, P, PAGNOTTA, E, PAINTER, M, PALAN, S, PALIT, IJ, PARK, A, GIL‐BAZO, J, PASCUAL, R, BACH, A, PASQUARIELLO, P, PASTOR, L, PATEL, V, PATTON, AJ, PEARSON, ND, PELIZZON, L, PELLI, M, PELSTER, M, GILDER, D, PÉRIGNON, C, PFIFFER, C, BAIDOO, E, PHILIP, R, PLÍHAL, T, PRAKASH, P, PRESS, O, PRODROMOU, T, PROKOPCZUK, M, PUTNINS, T, GLOSTEN, LR, QIAN, Y, RAIZADA, G, RAKOWSKI, D, BAKALLI, G, RANALDO, A, REGIS, L, REITZ, S, RENAULT, T, RENJIE, RW, RENO, R, GOMEZ, T, RIDDIOUGH, SJ, RINNE, K, RINTAMÄKI, P, RIORDAN, R, BAO, L, RITTMANNSBERGER, T, LONGARELA, IR, ROESCH, D, ROGNONE, L, ROSEMAN, B, GORBENKO, A, ROŞU, I, ROY, S, RUDOLF, N, RUSH, SR, RZAYEV, K, BARBON, A, RZEŹNIK, AA, SANFORD, A, SANKARAN, H, SARKAR, A, GRAMMIG, J, SARNO, L, SCAILLET, O, SCHARNOWSKI, S, SCHENK‐HOPPÉ, KR, SCHERTLER, A, SCHNEIDER, M, BASHCHENKO, O, SCHROEDER, F, SCHÜRHOFF, N, SCHUSTER, P, GRÉGOIRE, V, SCHWARZ, MA, SEASHOLES, MS, SEEGER, NJ, SHACHAR, O, SHKILKO, A, SHUI, J, SIKIC, M, BINDRA, PC, SIMION, G, SMALES, LA, GÜÇBILMEZ, U, SÖDERLIND, P, SOJLI, E, SOKOLOV, K, SÖNKSEN, J, SPOKEVICIUTE, L, STEFANOVA, D, SUBRAHMANYAM, MG, SZASZI, B, BJØNNES, GH, TALAVERA, O, ADRIAN, T, TANG, Y, TAYLOR, N, THAM, W, THEISSEN, E, THIMME, J, TONKS, I, TRAN, H, TRAPIN, L, TROLLE, AB, BLACK, JR, HAGSTRÖMER, B, VADUVA, MA, VALENTE, G, VAN NESS, RA, VASQUEZ, A, VEROUSIS, T, VERWIJMEREN, P, VILHELMSSON, A, VILKOV, G, VLADIMIROV, V, VOGEL, S, HAMBUCKERS, J, BLACK, BS, VOIGT, S, WAGNER, W, WALTHER, T, WEISS, P, VAN DER WEL, M, WERNER, IM, WESTERHOLM, PJ, WESTHEIDE, C, WIKA, HC, HAPNES, E, WIPPLINGER, E, BOGOEV, D, WOLF, M, WOLFF, CCP, WOLK, L, WONG, W, WRAMPELMEYER, J, WU, Z, XIA, S, XIU, D, HARRIS, JH, XU, K, XU, C, CORREA, SB, YADAV, PK, YAGÜE, J, YAN, C, YANG, A, YOO, W, YU, W, YU, Y, HARRIS, L, YU, S, YUESHEN, BZ, YUFEROVA, D, BONDARENKO, O, ZAMOJSKI, M, ZAREEI, A, ZEISBERGER, SM, ZHANG, L, ZHANG, SS, ZHANG, X, HARTMANN, S, ZHAO, L, ZHONG, Z, ZHOU, ZI, ZHOU, C, BOS, CS, ZHU, XS, ZOICAN, M, ZWINKELS, R, BOSCH‐ROSA, C, BOURI, E, HASSE, J, BROWNLEES, C, CALAMIA, A, CAO, VN, CAPELLE‐BLANCARD, G, ROMERO, LMC, CAPORIN, M, CARRION, A, CASKURLU, T, CHAKRABARTY, B, CHEN, J, HAUTSCH, N, CHERNOV, M, CHEUNG, W, CHINCARINI, LB, CHORDIA, T, CHOW, S, CLAPHAM, B, COLLIARD, J, COMERTON‐FORDE, C, CURRAN, E, DAO, T, HE, X, DARE, W, DAVIES, RJ, DE BLASIS, R, DE NARD, GF, DECLERCK, F, DEEV, O, DEGRYSE, H, DEKU, SY, DESAGRE, C, VAN DIJK, MA, HEATH, D, DIM, C, DIMPFL, T, DONG, YJ, DRUMMOND, PA, DUDDA, T, DUEVSKI, T, DUMITRESCU, A, DYAKOV, T, DYHRBERG, AH, DZIELIŃSKI, M, AIT‐SAHALIA, Y, EKSI, A, KALAK, IE, ELLEN, ST, EUGSTER, N, EVANS, MDD, FARRELL, M, FELEZ‐VINAS, E, FERRARA, G, FERROUHI, EM, FLORI, A, HEDIGER, S, FLUHARTY‐JAIDEE, JT, FOLEY, SDV, FONG, KYL, FOUCAULT, T, FRANUS, T, FRANZONI, F, FRIJNS, B, FRÖMMEL, M, FU, SM, FÜLLBRUNN, SC, HENDERSHOTT, T, GAN, B, GAO, G, GEHRIG, TP, HIBBERT, AM, HJALMARSSON, E, HOELSCHER, SA, HOFFMANN, P, HOLDEN, CW, HORENSTEIN, AR, HUANG, W, HUANG, D, AKMANSOY, O, HURLIN, C, ILCZUK, K, IVASHCHENKO, A, IYER, SR, JAHANSHAHLOO, H, JALKH, N, JONES, CM, JURKATIS, S, JYLHÄ, P, KAECK, AT, ALCOCK, JT, KAISER, G, KARAM, A, KARMAZIENE, E, KASSNER, B, KAUSTIA, M, KAZAK, E, KEARNEY, F, VAN KERVEL, V, KHAN, SA, KHOMYN, MK, ALEXEEV, V, KLEIN, T, KLEIN, O, KLOS, A, KOETTER, M, KOLOKOLOV, A, KORAJCZYK, RA, KOZHAN, R, KRAHNEN, JP, KUHLE, P, KWAN, A, ALOOSH, A, LAJAUNIE, Q, LAM, FYEC, LAMBERT, M, LANGLOIS, H, LAUSEN, J, LAUTER, T, LEIPPOLD, M, LEVIN, V, LI, Y, LI, H, AMATO, L, LIEW, CY, LINDNER, T, LINTON, O, LIU, J, LIU, A, LLORENTE, G, LOF, M, LOHR, A, LONGSTAFF, F, LOPEZ‐LIRA, A, AMAYA, D, and MANKAD, S
Abstract: ABSTRACTIn statistics, samples are drawn from a population in a data‐generating process (DGP). Standard errors measure the uncertainty in estimates of population parameters. In science, evidence is generated to test hypotheses in an evidence‐generating process (EGP). We claim that EGP variation across researchers adds uncertainty—nonstandard errors (NSEs). We study NSEs by letting 164 teams test the same hypotheses on the same data. NSEs turn out to be sizable, but smaller for more reproducible or higher rated research. Adding peer‐review stages reduces NSEs. We further find that this type of uncertainty is underestimated by participants.
Published: 2024

3. Non-Standard Errors

Author: Menkveld, AJ, Dreber, A, Holzmeister, F, Huber, J, Johanneson, M, Kirchler, M, Razen, M, Weitzel, U, Abad, D, Abudy, MM, Adrian, T, Gregoire, V, Hagströmer, B, Hambuckers, J, Hapnes, E, Harris, JH, Harris, L, Hartmann, S, Hasse, J-B, Hautsch, N, He, X-ZT, Ait-Sahalia, Y, Heath, D, Hediger, S, Hendershott, TJ, Hibbert, AM, Hjalmarsson, E, Hoelscher, S, Hoffmann, P, Holden, CW, Horenstein, AR, Huang, W, Akmansoy, O, Huang, D, Hurlin, C, Ivashchenko, A, Iyer, SR, Jahanshahloo, H, Jalkh, N, Jones, CM, Jurkatis, S, Jylha, P, Kaeck, A, Alcock, J, Kaiser, G, Karam, A, Karmaziene, E, Kassner, B, Kaustia, M, Kazak, E, Kearney, F, van Kervel, V, Khan, S, Khomyn, M, Alexeev, V, Klein, T, Klein, O, Klos, A, Koetter, M, Krahnen, JP, Kolokolov, A, Korajczyk, RA, Kozhan, R, Kwan, A, Lajaunie, Q, Aloosh, A, Lam, FYEC, Lambert, M, Langlois, H, Lausen, J, Lauter, T, Leippold, M, Levin, V, Li, Y, Li, MH, Liew, CY, Amato, L, Lindner, T, Linton, OB, Liu, J, Liu, A, Llorente-Alvarez, J-G, Lof, M, Lohr, A, Longstaff, FA, Lopez-Lira, A, Mankad, S, Amaya, D, Mano, N, Marchal, A, Martineau, C, Mazzola, F, Meloso, DC, Mihet, R, Mohan, V, Moinas, S, Moore, D, Mu, L, Angel, JJ, Muravyev, D, Murphy, D, Neszveda, G, Neumeier, C, Nielsson, U, Nimalendran, M, Nolte, S, Nordén, LL, O'Neill, P, Obaid, K, Bach, A, Ødegaard, BA, Östberg, P, Painter, M, Palan, S, Palit, I, Park, A, Pascual Gascó, R, Pasquariello, P, Pastor, L, Patel, V, Baidoo, E, Patton, AJ, Pearson, ND, Pelizzon, L, Pelster, M, Pérignon, C, Pfiffer, C, Philip, R, Plíhal, T, Prakash, P, Press, O-A, Bakalli, G, Prodromou, T, Putnins, TJ, Raizada, G, Rakowski, DA, Ranaldo, A, Regis, L, Reitz, S, Renault, T, Wang, R, Renò, R, Barbon, A, Riddiough, S, Rinne, K, Rintamäki, P, Riordan, R, RITTMANNSBERGER, T, Rodríguez Longarela, I, Rösch, D, Rognone, L, Roseman, B, Rosu, I, Bashchenko, O, Roy, S, Rudolf, N, Rush, S, Rzayev, K, Rzeźnik, A, Sanford, A, Sankaran, H, Sarkar, A, Sarno, L, Scaillet, O, Bindra, PC, Scharnowski, S, Schenk-Hoppé, KR, Schertler, A, Schneider, M, Schroeder, F, Schürhoff, N, Schuster, P, Schwarz, MA, Seasholes, MS, Seeger, N, Bjonnes, GH, Shachar, O, Shkilko, A, Shui, J, Sikic, M, Simion, G, Smales, LA, Söderlind, P, Sojli, E, Sokolov, K, Spokeviciute, L, Black, JR, Stefanova, D, Subrahmanyam, MG, Neusüss, S, Szaszi, B, Talavera, O, Tang, Y, Taylor, N, Tham, WW, Theissen, E, Thimme, J, Black, BS, Tonks, I, Tran, H, Trapin, L, Trolle, AB, Vaduva, M, Valente, G, Van Ness, RA, Vasquez, A, Verousis, T, Verwijmeren, P, Bohorquez, S, Vilhelmsson, A, Vilkov, G, Vladimirov, V, Vogel, S, Voigt, S, Wagner, W, Walther, T, Weiss, P, van der Wel, M, Werner, IM, Bondarenko, O, Westerholm, PJ, Westheide, C, Wipplinger, E, Wolf, M, Wolff, CCP, Wolk, L, Wong, WK, Wrampelmeyer, J, Wu, Z-X, Xia, S, Bos, CS, Xiu, D, Xu, K, Xu, C, Yadav, PK, Yagüe, J, Yan, C, Yang, A, Yoo, W, Yu, W, Yu, S, Bosch-Rosa, C, Yueshen, BZ, Yuferova, D, Zamojski, M, Zareei, A, Zeisberger, S, Zhang, S, Zhang, X, Zhong, Z, Zhou, ZI, Zhou, C, Bouri, E, Zhu, X, Zoican, M, Zwinkels, RCJ, Chen, J, Duevski, T, Gao, G, Gemayel, R, Gilder, D, Kuhle, P, Pagnotta, E, Brownlees, CT, Pelli, M, Sönksen, J, Zhang, L, Ilczuk, K, Bogoev, D, Qian, Y, Wika, HC, Yu, Y, Zhao, L, Mi, M, Calamia, A, Bao, L, Cao, VN, Capelle-Blancard, G, Capera, L, Caporin, M, Carrion, A, Caskurlu, T, Chakrabarty, B, Chernov, M, Cheung, WMY, Chincarini, LB, Chordia, T, Chow, SC, Clapham, B, Colliard, J-E, Comerton-Forde, C, Curran, E, Dao, T, Dare, W, Davies, RJ, De Blasis, R, De Nard, G, Declerck, F, Deev, O, Degryse, H, Deku, S, Desagre, C, Van Dijk, MA, Dim, C, Dimpfl, T, Dong, YJ, Drummond, P, Dudda, T, Dumitrescu, A, Dyakov, T, Dyhrberg, AH, Dzieliński, M, Eksi, A, El Kalak, I, ter Ellen, S, Eugster, N, Evans, MDD, Farrell, M, Félez-Viñas, E, Ferrara, G, FERROUHI, EM, Flori, A, Fluharty-Jaidee, J, Foley, S, Fong, KYL, Foucault, T, Franus, T, Franzoni, FA, Frijns, B, Frömmel, M, Fu, S, Füllbrunn, S, Gan, B, Gehrig, T, Gerritsen, D, Gil-Bazo, J, Glosten, LR, Gomez, T, Gorbenko, A, Güçbilmez, U, Grammig, J, Menkveld, AJ, Dreber, A, Holzmeister, F, Huber, J, Johanneson, M, Kirchler, M, Razen, M, Weitzel, U, Abad, D, Abudy, MM, Adrian, T, Gregoire, V, Hagströmer, B, Hambuckers, J, Hapnes, E, Harris, JH, Harris, L, Hartmann, S, Hasse, J-B, Hautsch, N, He, X-ZT, Ait-Sahalia, Y, Heath, D, Hediger, S, Hendershott, TJ, Hibbert, AM, Hjalmarsson, E, Hoelscher, S, Hoffmann, P, Holden, CW, Horenstein, AR, Huang, W, Akmansoy, O, Huang, D, Hurlin, C, Ivashchenko, A, Iyer, SR, Jahanshahloo, H, Jalkh, N, Jones, CM, Jurkatis, S, Jylha, P, Kaeck, A, Alcock, J, Kaiser, G, Karam, A, Karmaziene, E, Kassner, B, Kaustia, M, Kazak, E, Kearney, F, van Kervel, V, Khan, S, Khomyn, M, Alexeev, V, Klein, T, Klein, O, Klos, A, Koetter, M, Krahnen, JP, Kolokolov, A, Korajczyk, RA, Kozhan, R, Kwan, A, Lajaunie, Q, Aloosh, A, Lam, FYEC, Lambert, M, Langlois, H, Lausen, J, Lauter, T, Leippold, M, Levin, V, Li, Y, Li, MH, Liew, CY, Amato, L, Lindner, T, Linton, OB, Liu, J, Liu, A, Llorente-Alvarez, J-G, Lof, M, Lohr, A, Longstaff, FA, Lopez-Lira, A, Mankad, S, Amaya, D, Mano, N, Marchal, A, Martineau, C, Mazzola, F, Meloso, DC, Mihet, R, Mohan, V, Moinas, S, Moore, D, Mu, L, Angel, JJ, Muravyev, D, Murphy, D, Neszveda, G, Neumeier, C, Nielsson, U, Nimalendran, M, Nolte, S, Nordén, LL, O'Neill, P, Obaid, K, Bach, A, Ødegaard, BA, Östberg, P, Painter, M, Palan, S, Palit, I, Park, A, Pascual Gascó, R, Pasquariello, P, Pastor, L, Patel, V, Baidoo, E, Patton, AJ, Pearson, ND, Pelizzon, L, Pelster, M, Pérignon, C, Pfiffer, C, Philip, R, Plíhal, T, Prakash, P, Press, O-A, Bakalli, G, Prodromou, T, Putnins, TJ, Raizada, G, Rakowski, DA, Ranaldo, A, Regis, L, Reitz, S, Renault, T, Wang, R, Renò, R, Barbon, A, Riddiough, S, Rinne, K, Rintamäki, P, Riordan, R, RITTMANNSBERGER, T, Rodríguez Longarela, I, Rösch, D, Rognone, L, Roseman, B, Rosu, I, Bashchenko, O, Roy, S, Rudolf, N, Rush, S, Rzayev, K, Rzeźnik, A, Sanford, A, Sankaran, H, Sarkar, A, Sarno, L, Scaillet, O, Bindra, PC, Scharnowski, S, Schenk-Hoppé, KR, Schertler, A, Schneider, M, Schroeder, F, Schürhoff, N, Schuster, P, Schwarz, MA, Seasholes, MS, Seeger, N, Bjonnes, GH, Shachar, O, Shkilko, A, Shui, J, Sikic, M, Simion, G, Smales, LA, Söderlind, P, Sojli, E, Sokolov, K, Spokeviciute, L, Black, JR, Stefanova, D, Subrahmanyam, MG, Neusüss, S, Szaszi, B, Talavera, O, Tang, Y, Taylor, N, Tham, WW, Theissen, E, Thimme, J, Black, BS, Tonks, I, Tran, H, Trapin, L, Trolle, AB, Vaduva, M, Valente, G, Van Ness, RA, Vasquez, A, Verousis, T, Verwijmeren, P, Bohorquez, S, Vilhelmsson, A, Vilkov, G, Vladimirov, V, Vogel, S, Voigt, S, Wagner, W, Walther, T, Weiss, P, van der Wel, M, Werner, IM, Bondarenko, O, Westerholm, PJ, Westheide, C, Wipplinger, E, Wolf, M, Wolff, CCP, Wolk, L, Wong, WK, Wrampelmeyer, J, Wu, Z-X, Xia, S, Bos, CS, Xiu, D, Xu, K, Xu, C, Yadav, PK, Yagüe, J, Yan, C, Yang, A, Yoo, W, Yu, W, Yu, S, Bosch-Rosa, C, Yueshen, BZ, Yuferova, D, Zamojski, M, Zareei, A, Zeisberger, S, Zhang, S, Zhang, X, Zhong, Z, Zhou, ZI, Zhou, C, Bouri, E, Zhu, X, Zoican, M, Zwinkels, RCJ, Chen, J, Duevski, T, Gao, G, Gemayel, R, Gilder, D, Kuhle, P, Pagnotta, E, Brownlees, CT, Pelli, M, Sönksen, J, Zhang, L, Ilczuk, K, Bogoev, D, Qian, Y, Wika, HC, Yu, Y, Zhao, L, Mi, M, Calamia, A, Bao, L, Cao, VN, Capelle-Blancard, G, Capera, L, Caporin, M, Carrion, A, Caskurlu, T, Chakrabarty, B, Chernov, M, Cheung, WMY, Chincarini, LB, Chordia, T, Chow, SC, Clapham, B, Colliard, J-E, Comerton-Forde, C, Curran, E, Dao, T, Dare, W, Davies, RJ, De Blasis, R, De Nard, G, Declerck, F, Deev, O, Degryse, H, Deku, S, Desagre, C, Van Dijk, MA, Dim, C, Dimpfl, T, Dong, YJ, Drummond, P, Dudda, T, Dumitrescu, A, Dyakov, T, Dyhrberg, AH, Dzieliński, M, Eksi, A, El Kalak, I, ter Ellen, S, Eugster, N, Evans, MDD, Farrell, M, Félez-Viñas, E, Ferrara, G, FERROUHI, EM, Flori, A, Fluharty-Jaidee, J, Foley, S, Fong, KYL, Foucault, T, Franus, T, Franzoni, FA, Frijns, B, Frömmel, M, Fu, S, Füllbrunn, S, Gan, B, Gehrig, T, Gerritsen, D, Gil-Bazo, J, Glosten, LR, Gomez, T, Gorbenko, A, Güçbilmez, U, and Grammig, J
Published: 2024

4. ALMA detection of [CII] 158 micron emission from a strongly lensed z=2 star-forming galaxy

Author: Schaerer, D., Boone, F., Jones, T., Dessauges-Zavadsky, M., Sklias, P., Zamojski, M., Cava, A., Richard, J., Ellis, R., Rawle, T. D., Egami, E., and Combes, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Our objectives are to determine the properties of the interstellar medium (ISM) and of star-formation in typical star-forming galaxies at high redshift. Following up on our previous multi-wavelength observations with HST, Spitzer, Herschel, and the Plateau de Bure Interferometer (PdBI), we have studied a strongly lensed z=2.013 galaxy, the arc behind the galaxy cluster MACS J0451+0006, with ALMA to measure the [CII] 158 micron emission line, one of the main coolants of the ISM. [CII] emission from the southern part of this galaxy is detected at 10 $\sigma$. Taking into account strong gravitational lensing, which provides a magnification of $\mu=49$, the intrinsic lensing-corrected [CII]158 micron luminosity is $L(CII)=1.2 \times 10^8 L_\odot$. The observed ratio of [CII]-to-IR emission, $L(CII)/L(FIR) \approx (1.2-2.4) \times 10^{-3}$, is found to be similar to that in nearby galaxies. The same also holds for the observed ratio $L(CII)/L(CO)=2.3 \times 10^3$, which is comparable to that of star-forming galaxies and active galaxy nuclei (AGN) at low redshift. We utilize strong gravitational lensing to extend diagnostic studies of the cold ISM to an order of magnitude lower luminosity ($L(IR) \sim (1.1-1.3) \times 10^{11} L_\odot$) and SFR than previous work at high redshift. While larger samples are needed, our results provide evidence that the cold ISM of typical high redshift galaxies has physical characteristics similar to normal star forming galaxies in the local Universe., Comment: 5 pages, 4 figures. Accepted for publication in Astronomy & Astrophysics, Letters
Published: 2015
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5. Molecular gas content in strongly-lensed z~1.5-3 star-forming galaxies with low IR luminosities

Author: Dessauges-Zavadsky, M., Zamojski, M., Schaerer, D., Combes, F., Egami, E., Swinbank, A. M., Richard, J., Sklias, P., Rawle, T. D., Rex, M., Kneib, J. -P., Boone, F., and Blain, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: To extend the molecular gas measurements to typical star-forming galaxies (SFGs) with SFR < 40 Msun yr^{-1} and M* < 2.5x10^{10} Msun at z~1.5-3, we have observed CO emission with the IRAM Plateau de Bure Interferometer and 30m telescope for five strongly-lensed galaxies selected from the Herschel Lensing Survey. These observations are combined with a compilation of CO measurements from the literature. We infer the luminosity correction factors r2,1 = 0.81+/-0.20 and r3,1 = 0.57+/-0.15 for the J=2 and J=3 CO transitions, respectively, valid for SFGs at z>1. The combined sample of CO-detected SFGs at z>1 shows a large spread in star formation efficiency (SFE), such that SFE extend beyond the low values of local spirals and overlap the distribution of z>1 sub-mm galaxies. We find that the spread in SFE (or equivalently in molecular gas depletion timescale) is due to primarily the specific star formation rate, but also stellar mass and redshift. Correlations of SFE with the offset from the main-sequence and the compactness of the starburst are less clear. The increase of the molecular gas depletion timescale with M* now revealed by low M* SFGs at z>1 and observed at z=0 is in contrast to the admitted constant molecular gas depletion timescale and the linear Kennicutt-Schmidt relation. We confirm an increase of the molecular gas fraction (fgas) from z~0.2 to z~1.2, followed by a very mild increase toward higher redshifts. At each redshift fgas shows a large dispersion due to the dependence of fgas on M*, producing a gradient of increasing fgas with decreasing M*. We provide the first measure of fgas of z>1 SFGs at the low-M* end (10^{9.4} < M*/Msun < 10^{9.9}), reaching a mean fgas = 0.69+/-0.18, which shows a clear fgas upturn. Finally, we find evidence for a non-universal dust-to-gas ratio among high-redshift SFGs and sub-mm galaxies, local spirals and ULIRGs with near-solar metallicities., Comment: 21 pages, 16 figures. Accepted in A&A
Published: 2014
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6. New constraints on dust emission and UV attenuation of z=6.5-7.5 galaxies from millimeter observations

Author: Schaerer, D., Boone, F., Zamojski, M., Staguhn, J., Dessauges-Zavadsky, M., Finkelstein, S., and Combes, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have targeted two recently discovered Lyman break galaxies (LBGs) to search for dust continuum and [CII] 158 micron line emission. The strongly lensed z~6.8 LBG A1703-zD1 behind the galaxy cluster Abell 1703, and the spectroscopically confirmed z=7.508 LBG z8-GND-5296 in the GOODS-N field have been observed with the Plateau de Bure interferometer (PdBI) at 1.2mm. These observations have been combined with those of three z>6.5 Lya emitters (named HCM6A, Himiko, and IOK-1), for which deep measurements were recently obtained with the PdBI and ALMA. [CII] is undetected in both galaxies, providing a deep upper limit for Abell1703-zD1, comparable to recent ALMA non-detections. Dust continuum emission from Abell1703-zD1 and z8-GND-5296 is not detected with an rms of 0.12 and 0.16 mJy/beam. From these non-detections we derive upper limits on their IR luminosity and star formation rate, dust mass, and UV attenuation. Thanks to strong gravitational lensing the limit for Abell1703-zD1 is probing the sub-LIRG regime ($L_{IR} <8.1 \times 10^{10}$ Lsun) and very low dust masses ($M_d<1.6 \times 10^7$ Msun). We find that all five galaxies are compatible with the Calzetti IRX-$\beta$ relation, their UV attenuation is compatible with several indirect estimates from other methods (the UV slope, extrapolation of the attenuation measured from the IR/UV ratio at lower redshift, and SED fits), and the dust-to-stellar mass ratio is not incompatible with that of galaxies from z=0 to 3. For their stellar mass the high-z galaxies studied here have an attenuation below the one expected from the mean relation of low redshift (z<1.5) galaxies. More and deeper (sub)-mm data are clearly needed to directly determine the UV attenuation and dust content of the dominant population of high-z star-forming galaxies and to establish more firmly their dependence on stellar mass, redshift, and other properties., Comment: 10 pages, 7 figures. Minor revisions. Accepted for publication in A&A
Published: 2014
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7. [CII] and 12CO(1-0) Emission Maps in HLSJ091828.6+514223: A Strongly Lensed Interacting System at z=5.24

Author: Rawle, T. D., Egami, E., Bussmann, R. S., Gurwell, M., Ivison, R. J., Boone, F., Combes, F., Danielson, A. L. R., Rex, M., Richard, J., Smail, I., Swinbank, A. M., Altieri, B., Blain, A. W., Clement, B., Dessauges-Zavadsky, M., Edge, A. C., Fazio, G. G., Jones, T., Kneib, J. -P., Omont, A., Perez-Gonzalez, P. G., Schaerer, D., Valtchanov, I., van der Werf, P. P., Walth, G., Zamojski, M., and Zemcov, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Submillimeter Array (SMA) [CII] 158um and Jansky Very Large Array (JVLA) $^{12}$CO(1-0) line emission maps for the bright, lensed, submillimeter source at $z=5.2430$ behind Abell 773: HLSJ091828.6+514223 (HLS0918). We combine these measurements with previously reported line profiles, including multiple $^{12}$CO rotational transitions, [CI], water and [NII], providing some of the best constraints on the properties of the interstellar medium (ISM) in a galaxy at $z>5$. HLS0918 has a total far-infrared (FIR) luminosity L_FIR(8-1000um) = (1.6$\pm$0.1)x10^14 L_sun/mu, where the total magnification mu_total = 8.9$\pm$1.9, via a new lens model from the [CII] and continuum maps. Despite a HyLIRG luminosity, the FIR continuum shape resembles that of a local LIRG. We simultaneously fit all of the observed spectral line profiles, finding four components which correspond cleanly to discrete spatial structures identified in the maps. The two most redshifted spectral components occupy the nucleus of a massive galaxy, with a source plane separation <1 kpc. The reddest dominates the continuum map (de-magnified L_FIR = (1.1$\pm$0.2)x10^13 L_sun), and excites strong water emission in both nuclear components via a powerful FIR radiation field from the intense star formation. A third star-forming component is most likely a region of a merging companion (dV ~ 500 km/s) exhibiting generally similar gas properties. The bluest component originates from a spatially distinct region, and photo-dissociation region (PDR) analysis suggests that it is lower density, cooler and forming stars less vigorously than the other components. Strikingly, it has very strong [NII] emission which may suggest an ionized, molecular outflow. This comprehensive view of gas properties and morphology in HLS0918 previews the science possible for a large sample of high-redshift galaxies once ALMA attains full sensitivity., Comment: 28 pages, 9 figures, accepted in ApJ
Published: 2013
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8. Star formation histories, extinction, and dust properties of strongly lensed z~1.5-3 star-forming galaxies from the Herschel Lensing Survey

Author: Sklias, P., Zamojski, M., Schaerer, D., Dessauges-Zavadsky, M., Egami, E., Rex, M., Rawle, T., Richard, J., Boone, F., Simpson, J. M., Smail, I., van der Werf, P., Altieri, B., and Kneib, J. P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Multi-wavelength, optical to IR/sub-mm observations of 5 strongly lensed galaxies identified by the Herschel Lensing Survey, plus two well-studied lensed galaxies, MS1512-cB58 and the Cosmic Eye, for which we also provide updated Herschel measurements, are used to determine the physical properties of z~1.5-3 star-forming galaxies close to or below the detection limits of blank fields. We constrain their stellar and dust content, determine star formation rates and histories, dust attenuation and extinction laws, and other related properties. We perform SED-fits of the full photometry of each object as well for the optical and infrared parts separately, exploring various parameters, including nebular emission. The IR observations and emission line measurements, where available, are used a posteriori constraints on the models. Besides the various stellar population models we explore, we use the observed IR/UV ratio to estimate the extinction and create "energy conserving models", that constrain most accurately the physical properties of our sources. Our sample has a median lensing-corrected IR luminosity ~ 3e11 Lsun, stellar masses between 2e9 and 2e11 Msun, and IR/UV luminosity ratios spanning a wide range. The dust masses of our galaxies are in the range 2 to 17e7 Msun, extending previous studies at the same redshift down to lower masses. We do not find any particular trend of the dust temperature Tdust with IR luminosity, suggesting an overall warmer dust regime at our redshift regardless of luminosity. Lensing enables us to study the detailed physical properties of individual IR-detected z~1.5-3 galaxies up to a factor ~10 fainter than achieved with deep blank field observations. We demonstrate that multi-wavelength observations combining stellar and dust emission can constrain star formation histories and extinction laws of star-forming galaxies., Comment: 27 pages, 19 figures
Published: 2013
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9. An extended Herschel drop-out source in the center of AS1063, a 'normal' dusty galaxy at z=6.1 or SZ substructures?

Author: Boone, F., Clément, B., Richard, J., Schaerer, D., Lutz, D., Weiß, A., Zemcov, M., Egami, E., Rawle, T. D., Walth, G. L., Kneib, J. -P., Combes, F., Smail, I., Swinbank, A. M., Altieri, B., Blain, A. W., Chapman, S., Dessauges-Zavadsky, M., Ivison, R. J., Knudsen, K. K., Omont, A., Pello, R., Pérez-González, P. G., Valtchanov, I., van der Werf, P., and Zamojski, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In the course of our 870um APEX/LABOCA follow up of the Herschel Lensing Survey we have detected a source in AS1063 (RXC J2248.7-4431), that has no counterparts in any of the Herschel PACS/SPIRE bands, it is a Herschel 'drop-out' with S_870/S_500>0.5. The 870um emission is extended and centered on the brightest cluster galaxy suggesting either a multiply imaged background source or substructure in the Sunyaev-Zel'dovich (SZ) increment due to inhomogeneities in the hot cluster gas of this merging cluster. We discuss both interpretations with emphasis on the putative lensed source. Based on the observed properties and on our lens model we find that this source could be the first SMG with a moderate far infrared luminosity (L_FIR<10^12 L_sol) detected so far at z>4. In deep HST observations we identified a multiply imaged z~6 source and we measured its spectroscopic redshift z=6.107 with VLT/FORS. This source could be associated with the putative SMG but it is most likely offset spatially by 10-30kpc and they could be interacting galaxies. With a FIR luminosity in the range [5-15]x10^{11} L_sol corresponding to a star formation rate in the range [80-260]M_sol/yr, this SMG would be more representative than the extreme starbursts usually detected at z>4. With a total magnification of ~25 it would open a unique window to the 'normal' dusty galaxies at the end of the epoch of reionization., Comment: accepted for publication in A&A
Published: 2013
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10. Spectral Energy Distributions of Type 1 AGN in the COSMOS Survey I - The XMM-COSMOS Sample

Author: Elvis, M., Hao, H., Civano, F., Brusa, M., Salvato, M., Bongiorno, A., Capak, P., Zamorani, G., Comastri, A., Jahnke, K., Lusso, E., Mainieri, V., Trump, J. R., Ho, L. C., Aussel, H., Cappelluti, N., Cisternas, M., Frayer, D., Gilli, R., Hasinger, G., Huchra, J. P., Impey, C. D., Koekemoer, A. M., Lanzuisi, G., Floc'h, E. Le, Lilly, S. J., Liu, Y., McCarthy, P., McCracken, H. J., Merloni, A., Roeser, H. J., Sanders, D. B., Sargent, M., Scoville, N., Schinnerer, E., Schiminovich, D., Silverman, J., Taniguchi, Y., Vignali, C., Urry, C. M., Zamojski, M. A., and Zatloukal, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The "Cosmic Evolution Survey" (COSMOS) enables the study of the Spectral Energy Distributions (SEDs) of Active Galactic Nuclei (AGN) because of the deep coverage and rich sampling of frequencies from X-ray to radio. Here we present a SED catalog of 413 X-ray (\xmm) selected type 1 (emission line FWHM$>2000$ km s$^{-1}$) AGN with Magellan, SDSS or VLT spectrum. The SEDs are corrected for the Galactic extinction, for broad emission line contributions, constrained variability, and for host galaxy contribution. We present the mean SED and the dispersion SEDs after the above corrections in the rest frame 1.4 GHz to 40 keV, and show examples of the variety of SEDs encountered. In the near-infrared to optical (rest frame $\sim 8\mu m$-- 4000\AA), the photometry is complete for the whole sample and the mean SED is derived from detections only. Reddening and host galaxy contamination could account for a large fraction of the observed SED variety. The SEDs are all available on-line., Comment: 22 pages, 22 figures, ApJ accepted, scheduled to be published October 20th, 2012, v758
Published: 2012
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11. Far infrared constraints on the contamination by dust obscured galaxies of high-z dropout searches

Author: Boone, F., Schaerer, D., Pello, R., Lutz, D., Weiss, A., Egami, E., Smail, I., Rex, M., Rawle, T., Ivison, R., Laporte, N., Beelen, A., Combes, F., Blain, A. W., Richard, J., Kneib, J. -P., Zamojski, M., Dessauges-Zavadsky, M., Altieri, B., van der Werf, P., Swinbank, M., Perez-Gonzalez, P. G., Clement, B., Nordon, R., Magnelli, B., and Menten, K. M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The spectral energy distributions (SED) of dusty galaxies at intermediate redshift may look similar to very high redshift galaxies in the optical/near infrared (NIR) domain. This can lead to the contamination of high redshift galaxy searches based on broad band optical/NIR photometry by lower redshift dusty galaxies as both kind of galaxies cannot be distinguished. The contamination rate could be as high as 50%. {This work shows how the far infrared (FIR) domain can help to recognize likely low-z interlopers in an optical/NIR search for high-z galaxies.} We analyse the FIR SEDs of two galaxies proposed as very high redshift ($z>7$) dropout candidates based on deep Hawk-I/VLT observations. The FIR SEDs are sampled with PACS/Herschel at 100 and 160\,$\mu$m, with SPIRE/Herschel at 250, 350 and 500\,$\mu$m and with LABOCA/APEX at 870\,$\mu$m. We find that redshifts $>7$ would imply extreme FIR SEDs (with dust temperatures $>100$\,K and FIR luminosities $>10^{13}$\,$L_{\odot}$). At z$\sim$2, instead, the SEDs of both sources would be compatible with that of typical ULIRGs/SMGs. Considering all the data available for these sources from visible to FIR we re-estimate the redshifts and we find $z\sim$1.6--2.5. Due to the strong spectral breaks observed in these galaxies, standard templates from the literature fail to reproduce the visible-near IR part of the SEDs even when additional extinction is included. These sources resemble strongly dust obscured galaxies selected in Spitzer observations with extreme visible-to-FIR colors, and the galaxy GN10 at $z=4$. Galaxies with similar SEDs could contaminate other high redshift surveys., Comment: Accepted for publication in A&A
Published: 2011
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12. The XMM-Newton Wide-Field Survey in the COSMOS field (XMM-COSMOS): demography and multiwavelength properties of obscured and unobscured luminous AGN

Author: Brusa, M., Civano, F., Comastri, A., Miyaji, T., Salvato, M., Zamorani, G., Cappelluti, N., Fiore, F., Hasinger, G., Mainieri, V., Merloni, A., Bongiorno, A., Capak, P., Elvis, M., Gilli, R., Hao, H., Jahnke, K., Koekemoer, A. M., Ilbert, O., Floc'h, E. Le, Lusso, E., Mignoli, M., Schinnerer, E., Silverman, J. D., Treister, E., Trump, J. D., Vignali, C., Zamojski, M., Aldcroft, T., Aussel, H., Bardelli, S., Bolzonella, M., Cappi, A., Caputi, K., Contini, T., Finoguenov, A., Fruscione, A., Garilli, B., Impey, C. D., Iovino, A., Iwasawa, K., Kampczyk, P., Kartaltepe, J., Kneib, J. P., Knobel, C., Kovac, K., Lamareille, F., Leborgne, J-F., Brun, V. Le, Fevre, O. Le, Lilly, S. J., Maier, C., McCracken, H. J., Pello, R., Peng, Y-J, Perez-Montero, E., de Ravel, L., Sanders, D., Scodeggio, M., Scoville, N. Z., Tanaka, M., Taniguchi, Y., Tasca, L., de la Torre, S., Tresse, L., Vergani, D., and Zucca, E.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the final optical identifications of the medium-depth (~60 ksec), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~800 X-ray sources down to limiting fluxes of ~5x10^{-16}, ~3x10^{-15}, and ~7x10^{-15} erg/cm2/s in the 0.5-2 keV, 2-10 keV and 5-10 keV bands, respectively. The work is complemented by an extensive collection of multi-wavelength data from 24 micron to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for ~50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24micron detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of logL_X>44.5 AGN is at z~2. Spectroscopically-identified obscured and unobscured AGN, as well as normal and starforming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high redshift (z>1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X>10^{44} erg s^{-1}) X-ray luminosity is ~15-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations., Comment: ApJ, in press. 59 pages, 14 figures, 2 Tables. A few typos corrected and a reference added. Table 2 is also available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release ; a version of the paper in ApJ format (27 pages) is available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release/brusa_xmmcosmos_optid.pdf
Published: 2010
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13. Detections of CO Molecular Gas in 24um-Bright ULIRGs at z~2 in the Spitzer First Look Survey

Author: Yan, Lin, Tacconi, L. ~J., Fiolet, N., Sajina, A., Omont, A., Lutz, D., Zamojski, M., Neri, R., Cox, P., and Dasyra, K. ~M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present CO observations of 9 ULIRGs at z~2 with S(24\mu m)>1mJy, previously confirmed with the mid-IR spectra in the Spitzer First Look Survey. All targets are required to have accurate redshifts from Keck/GEMINI near-IR spectra. Using the Plateau de Bure millimeter-wave Interferometer (PdBI) at IRAM, we detect CO J(3-2) [7 objects] or J(2-1) [1 object] line emission from 8 sources with integrated intensities Ic ~(5-9)sigma. The CO detected sources have a variety of mid-IR spectra, including strong PAH, deep silicate absorption and power-law continuum, implying that these molecular gas rich objects at z~2 could be either starbursts or dust obscured AGNs. The measured line luminosity L'[CO] is (1.28-3.77)e+10[K km/s pc^2]. The averaged molecular gas mass M(H2) is 1.7e+10Msun, assuming CO-to-H2 conversion factor of 0.8Msun/[K km/s pc^2]. Three sources (33%) -- MIPS506, MIPS16144 & MIPS8342 -- have double peak velocity profiles. The CO double peaks in MIPS506 and MIPS16144 show spatial separations of 45kpc and 10.9kpc, allowing the estimates of the dynamical masses of 3.2e+11*sin^(-2)(i)Msun and 5.4e+11*sin^{-2}(i)Msun respectively. The implied gas fraction, M(gas)/M(dyn), is 3% and 4%, assuming an average inclination angle. Finally, the analysis of the HST/NIC2 images, mid-IR spectra and IR SED revealed that most of our sources are mergers, containing dust obscured AGNs dominating the luminosities at (3-6)um. Together, these results provide some evidence suggesting SMGs, bright 24um z~2 ULIRGs and QSOs could represent three different stages of a single evolutionary sequence, however, a complete physical model would require much more data, especially high spatial resolution spectroscopy., Comment: 15 pages, 8 figures, accepted for publication in ApJ.
Published: 2010
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14. The optical spectra of Spitzer 24 micron galaxies in the COSMOS field: II. Faint infrared sources in the zCOSMOS-bright 10k catalogue

Author: Caputi, K. I., Lilly, S. J., Aussel, H., Floc'h, E. Le, Sanders, D., Maier, C., Frayer, D., Carollo, C. M., Contini, T., Kneib, J. -P., Fevre, O. Le, Mainieri, V., Renzini, A., Scodeggio, M., Scoville, N., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Coppa, G., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Ilbert, O., Iovino, A., Kampczyk, P., Kartaltepe, J., Knobel, C., Kovac, K., Lamareille, F., Borgne, J. -F. Le, Brun, V. Le, Mignoli, M., Peng, Y., Perez-Montero, E., Ricciardelli, E., Salvato, M., Silverman, J., Surace, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Abbas, U., Bottini, D., Capak, P., Cappi, A., Cassata, P., Cimatti, A., Elvis, M., Hasinger, G., Koekemoer, A. M., Leauthaud, A., Maccagni, D., Marinoni, C., McCracken, H., Memeo, P., Meneux, B., Oesch, P., Pello, R., Porciani, C., Pozzetti, L., Scaramella, R., Scarlata, C., Schiminovich, D., Taniguchi, Y., and Zamojski, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have used the zCOSMOS-bright 10k sample to identify 3244 Spitzer/MIPS 24-micron-selected galaxies with 0.06< S(24um)< 0.50 mJy and I(AB)<22.5, over 1.5 deg^2 of the COSMOS field, and studied different spectral properties, depending on redshift. At 0.2
Published: 2009
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15. Galaxy Stellar Mass Assembly between 0.2<z<2 from the S-COSMOS survey

Author: Ilbert, O., Salvato, M., Floc'h, E. Le, Aussel, H., Capak, P., McCracken, H. J., Mobasher, B., Kartaltepe, J., Scoville, N., Sanders, D. B., Arnouts, S., Bundy, K., Cassata, P., Kneib, J. -P., Koekemoer, A., Fevre, O. Le, Lilly, S., Surace, J., Taniguchi, Y., Tasca, L., Thompson, D., Tresse, L., Zamojski, M., Zamorani, G., and Zucca, E.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We follow the galaxy stellar mass assembly by morphological and spectral type in the COSMOS 2-deg^2 field. We derive the stellar mass functions and stellar mass densities from z=2 to z=0.2 using 196,000 galaxies selected at F(3.6 micron) > 1 microJy with accurate photometric redshifts (sigma_((zp-zs)/(1+zs))=0.008 at i<22.5). Using a spectral classification, we find that z~1 is an epoch of transition in the stellar mass assembly of quiescent galaxies. Their stellar mass density increases by 1.1 dex between z=1.5-2 and z=0.8-1 (Delta t ~2.5 Gyr), but only by 0.3 dex between z=0.8-1 and z~0.1 (Delta t ~ 6 Gyr). Then, we add the morphological information and find that 80-90% of the massive quiescent galaxies (log(M)~11) have an elliptical morphology at z<0.8. Therefore, a dominant mechanism links the shutdown of star formation and the acquisition of an elliptical morphology in massive galaxies. Still, a significant fraction of quiescent galaxies present a Spi/Irr morphology at low mass (40-60% at log(M)~9.5), but this fraction is smaller than predicted by semi-analytical models using a ``halo quenching'' recipe. We also analyze the evolution of star-forming galaxies and split them into ``intermediate activity'' and ``high activity'' galaxies. We find that the most massive ``high activity'' galaxies end their high star formation rate phase first. Finally, the space density of massive star-forming galaxies becomes lower than the space density of massive elliptical galaxies at z<1. As a consequence, the rate of ``wet mergers'' involved in the formation of the most massive ellipticals must decline very rapidly at z<1, which could explain the observed slow down in the assembly of these quiescent and massive sources., Comment: 37 pages, 29 figures, accepted for publication in ApJ
Published: 2009
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16. Photometric redshift and classification for the XMM-COSMOS sources

Author: Salvato, M., Hasinger, G., Ilbert, O., Zamorani, G., Brusa, M., Scoville, N., Rau, A., Capak, P., Arnouts, S., Aussel, H., Bolzonella, M., Buongiorno, A., Cappelluti, N., Caputi, K., Civano, F., Cook, R., Elvis, M., Gilli, R., Jahnke, K., Kartaltepe, J. S., Impey, C. D., Lamareille, F., Floch, E. Le, Lilly, S., Mainieri, V., McCarthy, P., McCracken, H., Mignoli, M., Mobasher, B., Murayama, T., Sasaki, S., Sanders, D. B., Schiminovich, D., Shioya, Y., Shopbell, P., Silvermann, J., Smolcic, V., Surace, J., Taniguchi, Y., Thompson, D., Trump, J. R., Urry, M., and Zamojski, M.
Subjects: Astrophysics
Abstract: We present photometric redshifts and spectral energy distribution (SED) classifications for a sample of 1542 optically identified sources detected with XMM in the COSMOS field. Our template fitting classifies 46 sources as stars and 464 as non-active galaxies, while the remaining 1032 require templates with an AGN contribution. High accuracy in the derived photometric redshifts was accomplished as the result of 1) photometry in up to 30 bands with high significance detections, 2) a new set of SED templates including 18 hybrids covering the far-UV to mid-infrared, which have been constructed by the combination of AGN and non-active galaxies templates, and 3) multi-epoch observations that have been used to correct for variability (most important for type 1 AGN). The reliability of the photometric redshifts is evaluated using the sub-sample of 442 sources with measured spectroscopic redshifts. We achieved an accuracy of $\sigma_{\Delta z/(1+z_{spec})} = 0.014$ for i$_{AB}^*<$22.5 ($\sigma_{\Delta z/(1+z_{spec})} \sim0.015$ for i$_{AB}^*<$24.5). The high accuracies were accomplished for both type 2 (where the SED is often dominated by the host galaxy) and type 1 AGN and QSOs out to $z=4.5$. The number of outliers is a large improvement over previous photometric redshift estimates for X-ray selected sources (4.0% and 4.8% outliers for i$_{AB}^*<$22.5 and i$_{AB}^*<$24.5, respectively). We show that the intermediate band photometry is vital to achieving accurate photometric redshifts for AGN, whereas the broad SED coverage provided by mid infrared (Spitzer/IRAC) bands is important to reduce the number of outliers for normal galaxies., Comment: Accepted for publication in ApJ
Published: 2008
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17. COSMOS Photometric Redshifts with 30-bands for 2-deg2

Author: Ilbert, O., Capak, P., Salvato, M., Aussel, H., McCracken, H. J., Sanders, D. B., Scoville, N., Kartaltepe, J., Arnouts, S., Floc'h, E. Le, Mobasher, B., Taniguchi, Y., Lamareille, F., Leauthaud, A., Sasaki, S., Thompson, D., Zamojski, M., Zamorani, G., Bardelli, S., Bolzonella, M., Bongiorno, A., Brusa, M., Caputi, K. I., Carollo, C. M., Contini, T., Cook, R., Coppa, G., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Garilli, B., Hasinger, G., Iovino, A., Kampczyk, P., Kneib, J. -P., Knobel, C., Kovac, K., Borgne, J. F. Le, Brun, V. Le, Fevre, O. Le, Lilly, S., Looper, D., Maier, C., Mainieri, V., Mellier, Y., Mignoli, M., Murayama, T., Pello, R., Peng, Y., Perez-Montero, E., Renzini, A., Ricciardelli, E., Schiminovich, D., Scodeggio, M., Shioya, Y., Silverman, J., Surace, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., and Zucca, E.
Subjects: Astrophysics
Abstract: We present accurate photometric redshifts in the 2-deg2 COSMOS field. The redshifts are computed with 30 broad, intermediate, and narrow bands covering the UV (GALEX), Visible-NIR (Subaru, CFHT, UKIRT and NOAO) and mid-IR (Spitzer/IRAC). A chi2 template-fitting method (Le Phare) was used and calibrated with large spectroscopic samples from VLT-VIMOS and Keck-DEIMOS. We develop and implement a new method which accounts for the contributions from emission lines (OII, Hbeta, Halpha and Ly) to the spectral energy distributions (SEDs). The treatment of emission lines improves the photo-z accuracy by a factor of 2.5. Comparison of the derived photo-z with 4148 spectroscopic redshifts (i.e. Delta z = zs - zp) indicates a dispersion of sigma_{Delta z/(1+zs)}=0.007 at i<22.5, a factor of 2-6 times more accurate than earlier photo-z in the COSMOS, CFHTLS and COMBO-17 survey fields. At fainter magnitudes i<24 and z<1.25, the accuracy is sigma_{Delta z/(1+zs)}=0.012. The deep NIR and IRAC coverage enables the photo-z to be extended to z~2 albeit with a lower accuracy (sigma_{Delta z/(1+zs)}=0.06 at i~24). The redshift distribution of large magnitude-selected samples is derived and the median redshift is found to range from z=0.66 at 22
Published: 2008
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18. Deep GALEX Imaging of the HST/COSMOS Field: A First Look at the Morphology of z~0.7 Star-forming Galaxies

Author: Zamojski, M. A., Schiminovich, D., Rich, R. M., Mobasher, B., Koekemoer, A. M., Capak, P., Taniguchi, Y., Sasaki, S. S., McCracken, H. J., Mellier, Y., Bertin, E., Aussel, H., Sanders, D. B., Fevre, O. Le, Ilbert, O., Salvato, M., Thompson, D. J., Kartaltepe, J. S., Scoville, N., Barlow, T. A., Forster, K., Friedman, P. G., Martin, D. C., Morrisey, P., Neff, S. G., Seibert, M., Small, T., Wyder, T. K., Bianchi, L., Donas, J., Heckman, T. M., Lee, Y. -W., Madore, B. F., Milliard, B., Szalay, A. S., Welsh, B. Y., and Yi, S. K.
Subjects: Astrophysics
Abstract: We present a study of the morphological nature of redshift z~0.7 star-forming galaxies using a combination of HST/ACS, GALEX and ground-based images of the COSMOS field. Our sample consists of 8,146 galaxies, 5,777 of which are detected in the GALEX near-ultraviolet band down to a limiting magnitude of 25.5 (AB). We make use of the UV to estimate star formation rates, correcting for the effect of dust using the UV-slope, and compute, from the ACS F814W images, the C,A,S,G,M20 morphological parameters for all objects in our sample. We observe a morphological bimodality in the galaxy population and show that it has a strong correspondence with the FUV - g color bimodality. We conclude that UV-optical color predominantly evolves concurrently with morphology. We observe many of the most star-forming galaxies to have morphologies approaching that of early-type galaxies, and interpret this as evidence that strong starburst events are linked to bulge growth and constitute a process through which galaxies can be brought from the blue to the red sequence while simultaneously modifying their morphology accordingly. We conclude that the red sequence has continued growing at z~<0.7. We also observe z~0.7 galaxies to have physical properties similar to that of local galaxies, except for higher star formation rates. Whence we infer that the dimming of star-forming galaxies is responsible for most of the evolution in the star formation rate density of the Universe since that redshift, although our data are also consistent with a mild number evolution. [abridged], Comment: 29 pages including 22 figures. Accepted for publication in ApJS COSMOS Special Issue. A copy of the paper with high resolution figures is available at http://www.astro.columbia.edu/~michel/galex_cosmos_paper.pdf
Published: 2007
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19. Non-Standard Errors

Author: Menkveld, A.J., Dreber, A., Holzmeister, F., Huber, J., Johannesson, M., Kirchler, M., Razen, M., Weitzel, G.U., Abad, D., Abudy, M., Adrian, T., Ait-Sahalia, Y., Akmansoy, O., Alcock, J., Alexeev, V., Aloosh, A., Amato, L., Amaya, D., Angel, J., Bach, A., Baidoo, E., Bakalli, G., Barbon, A., Bashchenko, O., Bindra, P.C., Bjonnes, G.H., Black, J., Black, B.S., Bohorquez, S., Bondarenko, O., Bos, C.S., Bosch-Rosa, C., Bouri, E., Brownlees, C.T., Calamia, A., Cao, V.N., Capelle-Blancard, G., Capera, L., Caporin, M., Carrion, A., Caskurlu, T., Chakrabarty, B., Chernov, M., Cheung, W.M., Chincarini, L.B., Chordia, T., Chow, S.C., Clapham, B., Colliard, J.-E., Comerton-Forde, C., Curran, E., Dao, T., Dare, W., Davies, R.J., Blasis, R. De, Nard, G. De, DeClerck, F., Deev, O., Degryse, H., Deku, S., Desagre, C., Dijk, M.A van, Dim, C., Dimpfl, T., Dong, Y., Drummond, P., Dudda, T., Dumitrescu, A., Dyakov, T., Dyhrberg, A.H., Dzieliński, M., Eksi, A., Kalak, I. El, Ellen, S. ter, Eugster, N., Evans, M.D.D., Farrell, M., Félez-Viñas, E., Ferrara, G., Ferrouhi, E.M., Flori, A., Fluharty-Jaidee, J., Foley, S., Fong, K.Y.L., Foucault, T., Franus, T., Franzoni, F.A., Frijns, B., Frömmel, M., Fu, S., Füllbrunn, S.C., Gan, B., Gehrig, T., Gerritsen, D., Gil-Bazo, J., Glosten, L.R., Gomez, T., Gorbenko, A., Güçbilmez, U., Grammig, J., Gregoire, V., Hagströmer, B., Hambuckers, J., Hapnes, E., Harris, J.H., Harris, L., Hartmann, S., Hasse, J.-B., Hautsch, N., He, X., Heath, D., Hediger, S., Hendershott, T., Hibbert, A.M., Hjalmarsson, E., Hoelscher, S.A., Hoffmann, P., Holden, C.W., Horenstein, A.R., Huang, W., Huang, D., Hurlin, C., Ivashchenko, A., Iyer, S.R., Jahanshahloo, H., Jalkh, N., Jones, C.M., Jurkatis, S., Jylha, P., Kaeck, A., Kaiser, G., Karam, A., Karmaziene, E., Kassner, B., Kaustia, M., Kazak, E., Kearney, F., Kervel, V. van, Khan, S., Khomyn, M., Klein, T., Klein, O., Klos, A., Koetter, M., Krahnen, J.P., Kolokolov, A., Korajczyk, R.A., Kozhan, R., Kwan, A., Lajaunie, Q., Lam, F.E.C., Lambert, M., Langlois, H., Lausen, J., Lauter, T., Leippold, M., Levin, V., Li, Y., Li, H., Liew, C.Y., Lindner, T., Linton, O.B., Liu, J., Liu, A., Llorente, G., Lof, M., Lohr, A., Longstaff, F.A., Lopez-Lira, A., Mankad, S., Mano, N., Marchal, A., Martineau, C., Mazzola, F., Meloso, D., Mihet, R., Mohan, V., Moinas, S., Moore, D., Mu, L., Muravyev, D., Murphy, D., Neszveda, G., Neumeier, C., Nielsson, U., Nimalendran, M., Nolte, S., Norden, L.L., O'Neill, P., Obaid, K., Ødegaard, B.A., Östberg, P., Painter, M., Palan, S., Palit, I., Park, A., Pascual, R., Pasquariello, P., Pastor, L., Patel, V., Patton, A.J., Pearson, N.D., Pelizzon, L., Pelster, M., Pérignon, C., Pfiffer, C., Philip, R., Plíhal, T., Prakash, P., Press, O.-A., Prodromou, T., Putniņš, T.J., Raizada, G., Rakowski, D.A., Ranaldo, A., Regis, L., Reitz, S., Renault, T., Renjie, R.W., Renò, R., Riddiough, S., Rinne, K., Rintamäki, P., Riordan, R., Rittmannsberger, T., Rodríguez-Longarela, I., Rösch, D., Rognone, L., Roseman, B., Rosu, I., Roy, S., Rudolf, N., Rush, S., Rzayev, K., Rzeźnik, A., Sanford, A., Sankaran, H., Sarkar, A., Sarno, L., Scaillet, O., Scharnowski, S., Schenk-Hoppé, K.R., Schertler, A., Schneider, M., Schroeder, F., Schürhoff, N., Schuster, P., Schwarz, M.A., Seasholes, M.S., Seeger, N., Shachar, O., Shkilko, A., Shui, J., Sikic, M., Simion, G., Smales, L.A., Söderlind, P., Sojli, E., Sokolov, K., Spokeviciute, L., Stefanova, D., Subrahmanyam, M.G., Neusüss, S., Szaszi, B., Talavera, O., Tang, Y., Taylor, N., Tham, W.W., Theissen, E., Thimme, J., Tonks, I., Tran, H., Trapin, L., Trolle, A.B., Valente, G., Ness, R.A. Van, Vasquez, A., Verousis, T., Verwijmeren, P., Vilhelmsson, A., Vilkov, G., Vladimirov, V., Vogel, S., Voigt, S., Wagner, W., Walther, T., Weiss, P., Wel, M. van der, Werner, I.M., Westerholm, P.J., Westheide, C., Wipplinger, E., Wolf, M., Wolff, C.C.P., Wolk, L., Wong, W.-K., Wrampelmeyer, J., Xia, S., Xiu, D., Xu, K., Xu, C., Yadav, P.K., Yagüe, J., Yan, C., Yang, A., Yoo, W., Yu, W., Yu, S., Yueshen, B.Z., Yuferova, D., Zamojski, M., Zareei, A., Zeisberger, S.M., Zhang, S.S., Zhang, X., Zhong, Z., Zhou, Z.I., Zhou, C., Zhu, X.S., Zoican, M., Zwinkels, R.C.J., Chen, J., Duevski, T., Gao, G., Gemayel, R., Gilder, D. de, Kuhle, P., Pagnotta, E., Pelli, M., Sönksen, J., Zhang, L., Ilczuk, K., Bogoev, D., Qian, Y., Wika, H.C., Yu, Y., Zhao, L., Mi, M., Bao, L., Vaduva, A., Prokopczuk, P., Avetikian, A., Wu, Z.-X., Menkveld, A.J., Dreber, A., Holzmeister, F., Huber, J., Johannesson, M., Kirchler, M., Razen, M., Weitzel, G.U., Abad, D., Abudy, M., Adrian, T., Ait-Sahalia, Y., Akmansoy, O., Alcock, J., Alexeev, V., Aloosh, A., Amato, L., Amaya, D., Angel, J., Bach, A., Baidoo, E., Bakalli, G., Barbon, A., Bashchenko, O., Bindra, P.C., Bjonnes, G.H., Black, J., Black, B.S., Bohorquez, S., Bondarenko, O., Bos, C.S., Bosch-Rosa, C., Bouri, E., Brownlees, C.T., Calamia, A., Cao, V.N., Capelle-Blancard, G., Capera, L., Caporin, M., Carrion, A., Caskurlu, T., Chakrabarty, B., Chernov, M., Cheung, W.M., Chincarini, L.B., Chordia, T., Chow, S.C., Clapham, B., Colliard, J.-E., Comerton-Forde, C., Curran, E., Dao, T., Dare, W., Davies, R.J., Blasis, R. De, Nard, G. De, DeClerck, F., Deev, O., Degryse, H., Deku, S., Desagre, C., Dijk, M.A van, Dim, C., Dimpfl, T., Dong, Y., Drummond, P., Dudda, T., Dumitrescu, A., Dyakov, T., Dyhrberg, A.H., Dzieliński, M., Eksi, A., Kalak, I. El, Ellen, S. ter, Eugster, N., Evans, M.D.D., Farrell, M., Félez-Viñas, E., Ferrara, G., Ferrouhi, E.M., Flori, A., Fluharty-Jaidee, J., Foley, S., Fong, K.Y.L., Foucault, T., Franus, T., Franzoni, F.A., Frijns, B., Frömmel, M., Fu, S., Füllbrunn, S.C., Gan, B., Gehrig, T., Gerritsen, D., Gil-Bazo, J., Glosten, L.R., Gomez, T., Gorbenko, A., Güçbilmez, U., Grammig, J., Gregoire, V., Hagströmer, B., Hambuckers, J., Hapnes, E., Harris, J.H., Harris, L., Hartmann, S., Hasse, J.-B., Hautsch, N., He, X., Heath, D., Hediger, S., Hendershott, T., Hibbert, A.M., Hjalmarsson, E., Hoelscher, S.A., Hoffmann, P., Holden, C.W., Horenstein, A.R., Huang, W., Huang, D., Hurlin, C., Ivashchenko, A., Iyer, S.R., Jahanshahloo, H., Jalkh, N., Jones, C.M., Jurkatis, S., Jylha, P., Kaeck, A., Kaiser, G., Karam, A., Karmaziene, E., Kassner, B., Kaustia, M., Kazak, E., Kearney, F., Kervel, V. van, Khan, S., Khomyn, M., Klein, T., Klein, O., Klos, A., Koetter, M., Krahnen, J.P., Kolokolov, A., Korajczyk, R.A., Kozhan, R., Kwan, A., Lajaunie, Q., Lam, F.E.C., Lambert, M., Langlois, H., Lausen, J., Lauter, T., Leippold, M., Levin, V., Li, Y., Li, H., Liew, C.Y., Lindner, T., Linton, O.B., Liu, J., Liu, A., Llorente, G., Lof, M., Lohr, A., Longstaff, F.A., Lopez-Lira, A., Mankad, S., Mano, N., Marchal, A., Martineau, C., Mazzola, F., Meloso, D., Mihet, R., Mohan, V., Moinas, S., Moore, D., Mu, L., Muravyev, D., Murphy, D., Neszveda, G., Neumeier, C., Nielsson, U., Nimalendran, M., Nolte, S., Norden, L.L., O'Neill, P., Obaid, K., Ødegaard, B.A., Östberg, P., Painter, M., Palan, S., Palit, I., Park, A., Pascual, R., Pasquariello, P., Pastor, L., Patel, V., Patton, A.J., Pearson, N.D., Pelizzon, L., Pelster, M., Pérignon, C., Pfiffer, C., Philip, R., Plíhal, T., Prakash, P., Press, O.-A., Prodromou, T., Putniņš, T.J., Raizada, G., Rakowski, D.A., Ranaldo, A., Regis, L., Reitz, S., Renault, T., Renjie, R.W., Renò, R., Riddiough, S., Rinne, K., Rintamäki, P., Riordan, R., Rittmannsberger, T., Rodríguez-Longarela, I., Rösch, D., Rognone, L., Roseman, B., Rosu, I., Roy, S., Rudolf, N., Rush, S., Rzayev, K., Rzeźnik, A., Sanford, A., Sankaran, H., Sarkar, A., Sarno, L., Scaillet, O., Scharnowski, S., Schenk-Hoppé, K.R., Schertler, A., Schneider, M., Schroeder, F., Schürhoff, N., Schuster, P., Schwarz, M.A., Seasholes, M.S., Seeger, N., Shachar, O., Shkilko, A., Shui, J., Sikic, M., Simion, G., Smales, L.A., Söderlind, P., Sojli, E., Sokolov, K., Spokeviciute, L., Stefanova, D., Subrahmanyam, M.G., Neusüss, S., Szaszi, B., Talavera, O., Tang, Y., Taylor, N., Tham, W.W., Theissen, E., Thimme, J., Tonks, I., Tran, H., Trapin, L., Trolle, A.B., Valente, G., Ness, R.A. Van, Vasquez, A., Verousis, T., Verwijmeren, P., Vilhelmsson, A., Vilkov, G., Vladimirov, V., Vogel, S., Voigt, S., Wagner, W., Walther, T., Weiss, P., Wel, M. van der, Werner, I.M., Westerholm, P.J., Westheide, C., Wipplinger, E., Wolf, M., Wolff, C.C.P., Wolk, L., Wong, W.-K., Wrampelmeyer, J., Xia, S., Xiu, D., Xu, K., Xu, C., Yadav, P.K., Yagüe, J., Yan, C., Yang, A., Yoo, W., Yu, W., Yu, S., Yueshen, B.Z., Yuferova, D., Zamojski, M., Zareei, A., Zeisberger, S.M., Zhang, S.S., Zhang, X., Zhong, Z., Zhou, Z.I., Zhou, C., Zhu, X.S., Zoican, M., Zwinkels, R.C.J., Chen, J., Duevski, T., Gao, G., Gemayel, R., Gilder, D. de, Kuhle, P., Pagnotta, E., Pelli, M., Sönksen, J., Zhang, L., Ilczuk, K., Bogoev, D., Qian, Y., Wika, H.C., Yu, Y., Zhao, L., Mi, M., Bao, L., Vaduva, A., Prokopczuk, P., Avetikian, A., and Wu, Z.-X.
Abstract: 31 mei 2023, Contains fulltext : 240328.pdf (Author’s version preprint ) (Open Access), In statistics, samples are drawn from a population in a data-generating process (DGP). Standard errors measure the uncertainty in sample estimates of population parameters. In science, evidence is generated to test hypotheses in an evidence-generating process (EGP). We claim that EGP variation across researchers adds uncertainty: non-standard errors. To study them, we let 164 teams test six hypotheses on the same sample. We find that non-standard errors are sizeable, on par with standard errors. Their size (i) co-varies only weakly with team merits, reproducibility, or peer rating, (ii) declines significantly after peer-feedback, and (iii) is underestimated by participants.
Published: 2023

20. Non-Standard Errors

Author: Menkveld, A.J., Dreber, A., Holzmeister, F., Huber, J., Johannesson, M., Kirchler, M., Razen, M., Weitzel, G.U., Abad, D., Abudy, M., Adrian, T., Ait-Sahalia, Y., Akmansoy, O., Alcock, J., Alexeev, V., Aloosh, A., Amato, L., Amaya, D., Angel, J., Bach, A., Baidoo, E., Bakalli, G., Barbon, A., Bashchenko, O., Bindra, P.C., Bjonnes, G.H., Black, J., Black, B.S., Bohorquez, S., Bondarenko, O., Bos, C.S., Bosch-Rosa, C., Bouri, E., Brownlees, C.T., Calamia, A., Cao, V.N., Capelle-Blancard, G., Capera, L., Caporin, M., Carrion, A., Caskurlu, T., Chakrabarty, B., Chernov, M., Cheung, W.M., Chincarini, L.B., Chordia, T., Chow, S.C., Clapham, B., Colliard, J.-E., Comerton-Forde, C., Curran, E., Dao, T., Dare, W., Davies, R.J., Blasis, R. De, Nard, G. De, DeClerck, F., Deev, O., Degryse, H., Deku, S., Desagre, C., Dijk, M.A van, Dim, C., Dimpfl, T., Dong, Y., Drummond, P., Dudda, T., Dumitrescu, A., Dyakov, T., Dyhrberg, A.H., Dzieliński, M., Eksi, A., Kalak, I. El, Ellen, S. ter, Eugster, N., Evans, M.D.D., Farrell, M., Félez-Viñas, E., Ferrara, G., Ferrouhi, E.M., Flori, A., Fluharty-Jaidee, J., Foley, S., Fong, K.Y.L., Foucault, T., Franus, T., Franzoni, F.A., Frijns, B., Frömmel, M., Fu, S., Füllbrunn, S.C., Gan, B., Gehrig, T., Gerritsen, D., Gil-Bazo, J., Glosten, L.R., Gomez, T., Gorbenko, A., Güçbilmez, U., Grammig, J., Gregoire, V., Hagströmer, B., Hambuckers, J., Hapnes, E., Harris, J.H., Harris, L., Hartmann, S., Hasse, J.-B., Hautsch, N., He, X., Heath, D., Hediger, S., Hendershott, T., Hibbert, A.M., Hjalmarsson, E., Hoelscher, S.A., Hoffmann, P., Holden, C.W., Horenstein, A.R., Huang, W., Huang, D., Hurlin, C., Ivashchenko, A., Iyer, S.R., Jahanshahloo, H., Jalkh, N., Jones, C.M., Jurkatis, S., Jylha, P., Kaeck, A., Kaiser, G., Karam, A., Karmaziene, E., Kassner, B., Kaustia, M., Kazak, E., Kearney, F., Kervel, V. van, Khan, S., Khomyn, M., Klein, T., Klein, O., Klos, A., Koetter, M., Krahnen, J.P., Kolokolov, A., Korajczyk, R.A., Kozhan, R., Kwan, A., Lajaunie, Q., Lam, F.E.C., Lambert, M., Langlois, H., Lausen, J., Lauter, T., Leippold, M., Levin, V., Li, Y., Li, H., Liew, C.Y., Lindner, T., Linton, O.B., Liu, J., Liu, A., Llorente, G., Lof, M., Lohr, A., Longstaff, F.A., Lopez-Lira, A., Mankad, S., Mano, N., Marchal, A., Martineau, C., Mazzola, F., Meloso, D., Mihet, R., Mohan, V., Moinas, S., Moore, D., Mu, L., Muravyev, D., Murphy, D., Neszveda, G., Neumeier, C., Nielsson, U., Nimalendran, M., Nolte, S., Norden, L.L., O'Neill, P., Obaid, K., Ødegaard, B.A., Östberg, P., Painter, M., Palan, S., Palit, I., Park, A., Pascual, R., Pasquariello, P., Pastor, L., Patel, V., Patton, A.J., Pearson, N.D., Pelizzon, L., Pelster, M., Pérignon, C., Pfiffer, C., Philip, R., Plíhal, T., Prakash, P., Press, O.-A., Prodromou, T., Putniņš, T.J., Raizada, G., Rakowski, D.A., Ranaldo, A., Regis, L., Reitz, S., Renault, T., Renjie, R.W., Renò, R., Riddiough, S., Rinne, K., Rintamäki, P., Riordan, R., Rittmannsberger, T., Rodríguez-Longarela, I., Rösch, D., Rognone, L., Roseman, B., Rosu, I., Roy, S., Rudolf, N., Rush, S., Rzayev, K., Rzeźnik, A., Sanford, A., Sankaran, H., Sarkar, A., Sarno, L., Scaillet, O., Scharnowski, S., Schenk-Hoppé, K.R., Schertler, A., Schneider, M., Schroeder, F., Schürhoff, N., Schuster, P., Schwarz, M.A., Seasholes, M.S., Seeger, N., Shachar, O., Shkilko, A., Shui, J., Sikic, M., Simion, G., Smales, L.A., Söderlind, P., Sojli, E., Sokolov, K., Spokeviciute, L., Stefanova, D., Subrahmanyam, M.G., Neusüss, S., Szaszi, B., Talavera, O., Tang, Y., Taylor, N., Tham, W.W., Theissen, E., Thimme, J., Tonks, I., Tran, H., Trapin, L., Trolle, A.B., Valente, G., Ness, R.A. Van, Vasquez, A., Verousis, T., Verwijmeren, P., Vilhelmsson, A., Vilkov, G., Vladimirov, V., Vogel, S., Voigt, S., Wagner, W., Walther, T., Weiss, P., Wel, M. van der, Werner, I.M., Westerholm, P.J., Westheide, C., Wipplinger, E., Wolf, M., Wolff, C.C.P., Wolk, L., Wong, W.-K., Wrampelmeyer, J., Xia, S., Xiu, D., Xu, K., Xu, C., Yadav, P.K., Yagüe, J., Yan, C., Yang, A., Yoo, W., Yu, W., Yu, S., Yueshen, B.Z., Yuferova, D., Zamojski, M., Zareei, A., Zeisberger, S.M., Zhang, S.S., Zhang, X., Zhong, Z., Zhou, Z.I., Zhou, C., Zhu, X.S., Zoican, M., Zwinkels, R.C.J., Chen, J., Duevski, T., Gao, G., Gemayel, R., Gilder, D. de, Kuhle, P., Pagnotta, E., Pelli, M., Sönksen, J., Zhang, L., Ilczuk, K., Bogoev, D., Qian, Y., Wika, H.C., Yu, Y., Zhao, L., Mi, M., Bao, L., Vaduva, A., Prokopczuk, P., Avetikian, A., Wu, Z.-X., Menkveld, A.J., Dreber, A., Holzmeister, F., Huber, J., Johannesson, M., Kirchler, M., Razen, M., Weitzel, G.U., Abad, D., Abudy, M., Adrian, T., Ait-Sahalia, Y., Akmansoy, O., Alcock, J., Alexeev, V., Aloosh, A., Amato, L., Amaya, D., Angel, J., Bach, A., Baidoo, E., Bakalli, G., Barbon, A., Bashchenko, O., Bindra, P.C., Bjonnes, G.H., Black, J., Black, B.S., Bohorquez, S., Bondarenko, O., Bos, C.S., Bosch-Rosa, C., Bouri, E., Brownlees, C.T., Calamia, A., Cao, V.N., Capelle-Blancard, G., Capera, L., Caporin, M., Carrion, A., Caskurlu, T., Chakrabarty, B., Chernov, M., Cheung, W.M., Chincarini, L.B., Chordia, T., Chow, S.C., Clapham, B., Colliard, J.-E., Comerton-Forde, C., Curran, E., Dao, T., Dare, W., Davies, R.J., Blasis, R. De, Nard, G. De, DeClerck, F., Deev, O., Degryse, H., Deku, S., Desagre, C., Dijk, M.A van, Dim, C., Dimpfl, T., Dong, Y., Drummond, P., Dudda, T., Dumitrescu, A., Dyakov, T., Dyhrberg, A.H., Dzieliński, M., Eksi, A., Kalak, I. El, Ellen, S. ter, Eugster, N., Evans, M.D.D., Farrell, M., Félez-Viñas, E., Ferrara, G., Ferrouhi, E.M., Flori, A., Fluharty-Jaidee, J., Foley, S., Fong, K.Y.L., Foucault, T., Franus, T., Franzoni, F.A., Frijns, B., Frömmel, M., Fu, S., Füllbrunn, S.C., Gan, B., Gehrig, T., Gerritsen, D., Gil-Bazo, J., Glosten, L.R., Gomez, T., Gorbenko, A., Güçbilmez, U., Grammig, J., Gregoire, V., Hagströmer, B., Hambuckers, J., Hapnes, E., Harris, J.H., Harris, L., Hartmann, S., Hasse, J.-B., Hautsch, N., He, X., Heath, D., Hediger, S., Hendershott, T., Hibbert, A.M., Hjalmarsson, E., Hoelscher, S.A., Hoffmann, P., Holden, C.W., Horenstein, A.R., Huang, W., Huang, D., Hurlin, C., Ivashchenko, A., Iyer, S.R., Jahanshahloo, H., Jalkh, N., Jones, C.M., Jurkatis, S., Jylha, P., Kaeck, A., Kaiser, G., Karam, A., Karmaziene, E., Kassner, B., Kaustia, M., Kazak, E., Kearney, F., Kervel, V. van, Khan, S., Khomyn, M., Klein, T., Klein, O., Klos, A., Koetter, M., Krahnen, J.P., Kolokolov, A., Korajczyk, R.A., Kozhan, R., Kwan, A., Lajaunie, Q., Lam, F.E.C., Lambert, M., Langlois, H., Lausen, J., Lauter, T., Leippold, M., Levin, V., Li, Y., Li, H., Liew, C.Y., Lindner, T., Linton, O.B., Liu, J., Liu, A., Llorente, G., Lof, M., Lohr, A., Longstaff, F.A., Lopez-Lira, A., Mankad, S., Mano, N., Marchal, A., Martineau, C., Mazzola, F., Meloso, D., Mihet, R., Mohan, V., Moinas, S., Moore, D., Mu, L., Muravyev, D., Murphy, D., Neszveda, G., Neumeier, C., Nielsson, U., Nimalendran, M., Nolte, S., Norden, L.L., O'Neill, P., Obaid, K., Ødegaard, B.A., Östberg, P., Painter, M., Palan, S., Palit, I., Park, A., Pascual, R., Pasquariello, P., Pastor, L., Patel, V., Patton, A.J., Pearson, N.D., Pelizzon, L., Pelster, M., Pérignon, C., Pfiffer, C., Philip, R., Plíhal, T., Prakash, P., Press, O.-A., Prodromou, T., Putniņš, T.J., Raizada, G., Rakowski, D.A., Ranaldo, A., Regis, L., Reitz, S., Renault, T., Renjie, R.W., Renò, R., Riddiough, S., Rinne, K., Rintamäki, P., Riordan, R., Rittmannsberger, T., Rodríguez-Longarela, I., Rösch, D., Rognone, L., Roseman, B., Rosu, I., Roy, S., Rudolf, N., Rush, S., Rzayev, K., Rzeźnik, A., Sanford, A., Sankaran, H., Sarkar, A., Sarno, L., Scaillet, O., Scharnowski, S., Schenk-Hoppé, K.R., Schertler, A., Schneider, M., Schroeder, F., Schürhoff, N., Schuster, P., Schwarz, M.A., Seasholes, M.S., Seeger, N., Shachar, O., Shkilko, A., Shui, J., Sikic, M., Simion, G., Smales, L.A., Söderlind, P., Sojli, E., Sokolov, K., Spokeviciute, L., Stefanova, D., Subrahmanyam, M.G., Neusüss, S., Szaszi, B., Talavera, O., Tang, Y., Taylor, N., Tham, W.W., Theissen, E., Thimme, J., Tonks, I., Tran, H., Trapin, L., Trolle, A.B., Valente, G., Ness, R.A. Van, Vasquez, A., Verousis, T., Verwijmeren, P., Vilhelmsson, A., Vilkov, G., Vladimirov, V., Vogel, S., Voigt, S., Wagner, W., Walther, T., Weiss, P., Wel, M. van der, Werner, I.M., Westerholm, P.J., Westheide, C., Wipplinger, E., Wolf, M., Wolff, C.C.P., Wolk, L., Wong, W.-K., Wrampelmeyer, J., Xia, S., Xiu, D., Xu, K., Xu, C., Yadav, P.K., Yagüe, J., Yan, C., Yang, A., Yoo, W., Yu, W., Yu, S., Yueshen, B.Z., Yuferova, D., Zamojski, M., Zareei, A., Zeisberger, S.M., Zhang, S.S., Zhang, X., Zhong, Z., Zhou, Z.I., Zhou, C., Zhu, X.S., Zoican, M., Zwinkels, R.C.J., Chen, J., Duevski, T., Gao, G., Gemayel, R., Gilder, D. de, Kuhle, P., Pagnotta, E., Pelli, M., Sönksen, J., Zhang, L., Ilczuk, K., Bogoev, D., Qian, Y., Wika, H.C., Yu, Y., Zhao, L., Mi, M., Bao, L., Vaduva, A., Prokopczuk, P., Avetikian, A., and Wu, Z.-X.
Abstract: Item does not contain fulltext, In statistics, samples are drawn from a population in a data-generating process (DGP). Standard errors measure the uncertainty in sample estimates of population parameters. In science, evidence is generated to test hypotheses in an evidence-generating process (EGP). We claim that EGP variation across researchers adds uncertainty: non-standard errors. To study them, we let 164 teams test six hypotheses on the same sample. We find that non-standard errors are sizeable, on par with standard errors. Their size (i) co-varies only weakly with team merits, reproducibility, or peer rating, (ii) declines significantly after peer-feedback, and (iii) is underestimated by participants.
Published: 2022

21. VizieR Online Data Catalog: COSMOS photometric redshift catalog (Ilbert+, 2009)

Author: Ilbert, O., Capak, P., Salvato, M., Aussel, H., Mccracken, H. J., Sanders, D. B., Scoville, N., Kartaltepe, J., Arnouts, S., Le Floc H, E., Mobasher, B., Taniguchi, Y., Lamareille, F., Leauthaud, A., Sasaki, S., Thompson, D., Zamojski, M., Zamorani, G., Bardelli, S., Bolzonella, M., Angela Bongiorno, Brusa, M., Caputi, K. I., Carollo, C. M., Contini, T., Cook, R., Coppa, G., Cucciati, O., La Torre, S., Ravel, L., Franzetti, P., Garilli, B., Hasinger, G., Iovino, A., Kampczyk, P., Kneib, J. -P, Knobel, C., Kovac, K., Le Borgne, J. F., Le Brun, V., Fevre, O. L., Lilly, S., Looper, D., Maier, C., Mainieri, V., Mellier, Y., Mignoli, M., Murayama, T., Pello, R., Peng, Y., Perez-Montero, E., Renzini, A., Ricciardelli, E., Schiminovich, D., Scodeggio, M., Shioya, Y., Silverman, J., Surace, J., Tanaka, M., Tasca, L., Tresse, L., Vergani, D., Zucca, E., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Photometry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Redshifts, Surveys, Galaxy catalogs
Published: 2017

22. Molecular gas properties of a lensed star‐forming galaxy at z similar to 3.6: a case study

Author: Dessauges‐Zavadsky, M., Zamojski, M., Rujopakarn, W., Richard, J., Sklias, P., Schaerer, D., Combes, F., Ebeling, H., Rawle, T. D., Egami, E., Boone, F., Clement, B., Kneib, J. ‐P., Nyland, K., Walth, G., Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), and Chaire Galaxies et cosmologie
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; We report on the galaxy MACSJ0032‐arc at z(CO) = 3.6314 discovered during the Herschel Lensing snapshot Survey of massive galaxy clusters, and strongly lensed by the cluster MACSJ0032.1+1808. The successful detections of its rest‐frame ultraviolet (UV), optical, far‐infrared (FIR), millimeter, and radio continua, and of its CO emission enable us to characterize, for the first time at such a high redshift, the stellar, dust, and molecular gas properties of a compact star‐forming galaxy with a size smaller than 2.5 kpc, a fairly low stellar mass of 4.8(‐1.0)(+0.5) x 10(9) M circle dot, and a moderate IR luminosity of 4.8(‐0.6)(+1.2) x 10(11) L circle dot. By combining the stretching effect of the lens with the high angular resolution imaging of the CO(10) line emission and the radio continuum at 5 GHz, we find that the bulk of the molecular gas mass and star formation seems to be spatially decoupled from the rest‐frame UV emission. About 90% of the total star formation rate is undetected at rest‐frame UV wavelengths because of severe obscuration by dust, but is seen through the thermal FIR dust emission and the radio synchrotron radiation. The observed CO(43) and CO(65) lines demonstrate that high‐J transitions, at least up to J = 6, remain excited in this galaxy, whose CO spectral line energy distribution resembles that of high‐redshift submm galaxies, even though the IR luminosity of MACSJ0032‐arc is ten times lower. This high CO excitation is possibly due to the compactness of the galaxy. We find evidence that this high CO excitation has to be considered in the balance when estimating the CO‐to‐H‐2 conversion factor. Indeed, the respective CO‐to‐H‐2 conversion factors as derived from the correlation with metallicity and the FIR dust continuum can only be reconciled if excitation is accounted for. The inferred depletion time of the molecular gas in MACSJ0032‐arc supports the decrease in the gas depletion timescale of galaxies with redshift, although to a lesser degree than predicted by galaxy evolution models. Instead, the measured molecular gas fraction as high as 6079% in MACSJ0032‐arc favors the continued increase in the gas fraction of galaxies with redshift as expected, despite the plateau observed between z similar to 1.5 and z similar to 2.5.
Published: 2017

23. Molecular gas properties of a lensed star-forming galaxy at z ~ 3.6: a case study

Author: Dessauges-Zavadsky, M., primary, Zamojski, M., additional, Rujopakarn, W., additional, Richard, J., additional, Sklias, P., additional, Schaerer, D., additional, Combes, F., additional, Ebeling, H., additional, Rawle, T. D., additional, Egami, E., additional, Boone, F., additional, Clément, B., additional, Kneib, J.-P., additional, Nyland, K., additional, and Walth, G., additional
Published: 2017
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24. Molecular gas content in strongly lensed z similar to 1.5-3 star-forming galaxies with low infrared luminosities

Author: Dessauges-Zavadsky, M., Zamojski, M., Schaerer, D., Combes, F., Egami, E., Swinbank, A. M., Richard, J., Sklias, P., Rawle, T. D., Rex, M., Kneib, J-P., Boone, F., Blain, A., Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Collège de France - Chaire Galaxies et cosmologie, Collège de France (CdF (institution)), Steward Observatory, University of Arizona, Department of Physics, Durham University, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Herschel Science Centre, Agence Spatiale Européenne = European Space Agency (ESA), Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), Services communs OMP (UMS 831), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), AUTRES, Department of Physics and Astronomy [Leicester], University of Leicester, Université de Genève (UNIGE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Chaire Galaxies et cosmologie, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), European Space Agency (ESA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: galaxies: high-redshift, cosmology: observations, gravitational lensing: strong, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ISM: molecules
Abstract: International audience; To extend the molecular gas measurements to more typical star-forming galaxies (SFGs) with star formation rates SFR \textless 40 M-circle dot yr(-1) and stellar masses M-* \textless 2.5 x 10(10) M-circle dot at z similar to 1.5-3, we have observed CO emission with the IRAM Plateau de Bure Interferometer and the IRAM 30 m telescope for five strongly lensed galaxies, selected from the Herschel Lensing Survey. These observations are combined with a compilation of CO measurements from the literature. From this, we infer the CO luminosity correction factors r(2,1) = 0.81 +/- 0.20 and r(3,1) = 0.57 +/- 0.15 for the J = 2 and J = 3 CO transitions, respectively, valid for SFGs at z \textgreater 1. The combined sample of CO-detected SFGs at z \textgreater 1 shows a large spread in star formation efficiency (SFE) with a dispersion of 0.33 dex, such that the SFE extends well beyond the low values of local spirals and overlaps the distribution of z \textgreater 1 submm galaxies. We find that the spread in SFE (or equivalently in molecular gas depletion timescale) is due to the variations of several physical parameters, primarily the specific star formation rate, and also stellar mass and redshift. The dependence of SFE on the offset from the main sequence and the compactness of the starburst is less clear. The possible increase of the molecular gas depletion timescale with stellar mass, now revealed by low M-* SFGs at z \textgreater 1 and also observed at z = 0, contrasts with the generally acknowledged constant molecular gas depletion timescale and refutes the linearity of the Kennicutt-Schmidt relation. A net rise of the molecular gas fraction (f(gas)) is observed from z similar to 0.2 to z similar to 1.2, followed by a very mild increase toward higher redshifts, as found in earlier studies. At each redshift the molecular gas fraction shows a large dispersion, mainly due to the dependence of f(gas) on stellar mass, producing a gradient of increasing f(gas) with decreasing M-*. We provide the first measurement of the molecular gas fraction of z \textgreater 1 SFGs at the low-M-* end between 10(9.4) \textless M-*/M-circle dot \textless 10(9.9), reaching a mean af(gas)o = 0.69 +/- 0.18, which shows a clear f(gas) upturn at these lower stellar masses. Finally, we find evidence for a nonuniversal dust-to-gas ratio among high-redshift SFGs, high-redshift submm galaxies, local spirals, and local ultraluminous IR galaxies with near-solar metallicities, as inferred from a homogeneous analysis of their rest-frame 850 mu m luminosity per unit gas mass. The SFGs with z \textgreater 1 show a trend for a lower L-nu(850 mu m)/M-gas mean by 0.33 dex compared to the other galaxy populations.
Published: 2015

25. The XMM-Newton Wide-Field Survey in the COSMOS field (XMM-COSMOS): demography and multiwavelength properties of obscured and unobscured luminous AGN

Author: BRUSA, MARCELLA, LUSSO, ELISABETA, VIGNALI, CRISTIAN, Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J. F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y. J, Perez Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., Zucca E., Brusa M., Civano F., Comastri A., Miyaji T., Salvato M., Zamorani G., Cappelluti N., Fiore F., Hasinger G., Mainieri V., Merloni A., Bongiorno A., Capak P., Elvis M., Gilli R., Hao H., Jahnke K., Koekemoer A. M., Ilbert O., Le Floc'h E., Lusso E., Mignoli M., Schinnerer E., Silverman J. D., Treister E., Trump J. D., Vignali C., Zamojski M., Aldcroft T., Aussel H., Bardelli S., Bolzonella M., Cappi A., Caputi K., Contini T., Finoguenov A., Fruscione A., Garilli B., Impey C. D., Iovino A., Iwasawa K., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leborgne J.-F., Le Brun V., Le Fevre O., Lilly S. J., Maier C., McCracken H. J., Pello R., Peng Y-J, Perez-Montero E., de Ravel L., Sanders D., Scodeggio M., Scoville N. Z., Tanaka M., Taniguchi Y., Tasca L., de la Torre S., Tresse L., Vergani D., and Zucca E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active – surveys – X-rays: diffuse background – X-rays: galaxies – X-rays: general, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the final optical identifications of the medium-depth (~60 ksec), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~800 X-ray sources down to limiting fluxes of ~5x10^{-16}, ~3x10^{-15}, and ~7x10^{-15} erg/cm2/s in the 0.5-2 keV, 2-10 keV and 5-10 keV bands, respectively. The work is complemented by an extensive collection of multi-wavelength data from 24 micron to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for ~50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24micron detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of logL_X>44.5 AGN is at z~2. Spectroscopically-identified obscured and unobscured AGN, as well as normal and starforming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high redshift (z>1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X>10^{44} erg s^{-1}) X-ray luminosity is ~15-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations., ApJ, in press. 59 pages, 14 figures, 2 Tables. A few typos corrected and a reference added. Table 2 is also available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release ; a version of the paper in ApJ format (27 pages) is available at http://www.mpe.mpg.de/XMMCosmos/xmm53_release/brusa_xmmcosmos_optid.pdf
Published: 2010
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26. The Optical Spectra of 24 μm Galaxies in the COSMOS Field. I. Spitzer MIPS Bright Sources in the zCOSMOS-Bright 10k Catalog

Author: Caputi K. I., Lilly S. J., Aussel H., Sanders D., Frayer D., Le Fèvre O., Renzini A., Zamorani G., Scodeggio M., Contini T., Scoville N., Carollo C. M., Hasinger G., Iovino A., Le Brun V., Le Floc'h E., Maier C., Mainieri V., Mignoli M., Salvato M., Schiminovich D., Silverman J., Surace J., Tasca L., Abbas U., Bardelli S., Bolzonella M., Bongiorno A., Bottini D., Capak P., Cappi A., Cassata P., de la Torre S., de Ravel L., Franzetti P., Fumana M., Garilli B., Halliday C., Ilbert O., Kampczyk P., Kartaltepe J., Kneib J. P., Knobel C., Kovac K., Lamareille F., Leauthaud A., Le Borgne J. F., Maccagni D., Marinoni C., McCracken H., Meneux B., Oesch P., Pellò R., Pérez Montero E., Porciani C., Ricciardelli E., Scaramella R., Scarlata C., Tresse L., Vergani D., Walcher J., Zamojski M., Zucca E., CIMATTI, ANDREA, CUCCIATI, OLGA, Caputi K. I., Lilly S. J., Aussel H., Sanders D., Frayer D., Le Fèvre O., Renzini A., Zamorani G., Scodeggio M., Contini T., Scoville N., Carollo C. M., Hasinger G., Iovino A., Le Brun V., Le Floc'h E., Maier C., Mainieri V., Mignoli M., Salvato M., Schiminovich D., Silverman J., Surace J., Tasca L., Abbas U., Bardelli S., Bolzonella M., Bongiorno A., Bottini D., Capak P., Cappi A., Cassata P., Cimatti A., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Fumana M., Garilli B., Halliday C., Ilbert O., Kampczyk P., Kartaltepe J., Kneib J.-P., Knobel C., Kovac K., Lamareille F., Leauthaud A., Le Borgne J. F., Maccagni D., Marinoni C., McCracken H., Meneux B., Oesch P., Pellò R., Pérez-Montero E., Porciani C., Ricciardelli E., Scaramella R., Scarlata C., Tresse L., Vergani D., Walcher J., Zamojski M., and Zucca E.
Abstract: We study zCOSMOS-bright optical spectra for 609 Spitzer MIPS 24 μm-selected galaxies with S24 μm > 0.30 mJy and I < 22.5 (AB mag) over 1.5 deg2 of the COSMOS field. From emission-line diagnostics we find the following: (1) SFRs derived from the observed Hα λ6563 and Hβ λ4861 lines underestimate, on average, the total SFR by factors of ∼5 and 10, respectively. (2) Both the Calzetti et al. and the Milky Way reddening laws are suitable to describe the extinction observed in IR sources in most cases. (3) Some IR galaxies at z < 0.3 have low abundances, but many others with similar IR luminosities and redshifts are chemically enriched. (4) The average [O III] λ5007/Hβ λ4861 ratios of vLv24 μm > 1011 L⊙ galaxies at 0.6 < z < 0.7 are ∼0.6 dex higher than the average ratio of all zCOSMOS galaxies at similar redshifts. Massive star formation and AGNs could simultaneously be present in those galaxies with the highest ionizing fluxes. (5) Roughly of the galaxies with metallicity measurements at 0.5 < z < 0.7 lie below the general mass-metallicity relation at the corresponding redshifts. The strengths of the 4000 Å break and the Hδ EW of our galaxies show that secondary bursts of star formation are needed to explain the spectral properties of most IR sources. The LIRG and ULIRG phases occur, on average, between 107 and 10 8 yr after the onset of a starburst on top of underlying older stellar populations. These results are valid for galaxies of different IR luminosities at 0.6 < z < 1.0 and seem independent of the mechanisms triggering star formation
Published: 2008

27. Spectral energy distributions of Type~1 AGN in the COSMOS survey I - The XMM-COSMOS sample

Author: Elvis M., Hao H., Civano F., Salvato M., Bongiorno A., Capak P., Zamorani G., Comastri A., Jahnke K., Mainieri V., Trump J. R., Ho L. C., Aussel A., Cappelluti N., Cisternas M., Frayer D., Gilli R., Hasinger G., Huchra J. P., Impey C. D., Koekemoer A. M., LANZUISI, GIORGIO, Le Floc'h E., Lilly S. J., Liu Y., McCarthy P., McCracken H. J., Merloni A., Roeser H. J., Sanders D. B., Sargent M., Scoville N., Schinnerer E., Schiminovich D., Silverman J., Taniguchi Y., Urry C. M., Zamojski M. A., Zatloukal M., BRUSA, MARCELLA, LUSSO, ELISABETA, VIGNALI, CRISTIAN, Elvis M., Hao H., Civano F., Brusa M., Salvato M., Bongiorno A., Capak P., Zamorani G., Comastri A., Jahnke K., Lusso E., Mainieri V., Trump J.R., Ho L.C., Aussel A., Cappelluti N., Cisternas M., Frayer D., Gilli R., Hasinger G., Huchra J.P., Impey C.D., Koekemoer A.M., Lanzuisi G., Le Floc'h E., Lilly S.J., Liu Y., McCarthy P., McCracken H.J., Merloni A., Roeser H.-J., Sanders D.B., Sargent M., Scoville N., Schinnerer E., Schiminovich D., Silverman J., Taniguchi Y., Vignali C., Urry C.M., Zamojski M.A., and Zatloukal M.
Subjects: surveys, Astrophysics::High Energy Astrophysical Phenomena, quasars: general, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: The "Cosmic Evolution Survey" (COSMOS) enables the study of the spectral energy distributions (SEDs) of active galactic nuclei (AGNs) because of the deep coverage and rich sampling of frequencies from X-ray to radio. Here we present an SED catalog of 413 X-ray (XMM-Newton)-selected type 1 (emission line FWHM > 2000 km s-1) AGNs with Magellan, SDSS, or VLT spectrum. The SEDs are corrected for Galactic extinction, broad emission line contributions, constrained variability, and host galaxy contribution. We present the mean SED and the dispersion SEDs after the above corrections in the rest-frame 1.4 GHz to 40 keV, and show examples of the variety of SEDs encountered. In the near-infrared to optical (rest frame ~8 μm-4000 Å), the photometry is complete for the whole sample and the mean SED is derived from detections only. Reddening and host galaxy contamination could account for a large fraction of the observed SED variety. The SEDs are all available online.
Published: 2012

28. EMphot \mdash Photometric Software with Bayesian Priors: Application to GALEX

Author: Conseil, S., Vibert, D., Amouts, S., Milliard, B., Zamojski, M., Llebaria, A., Guillaume, Marion, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Evans, I.~N. and Accomazzi, A. and Mink, D.~J. and Rots, A.~H., Surace, Christian, and Evans, I.~N. and Accomazzi, A. and Mink, D.~J. and Rots, A.~H.
Subjects: [INFO]Computer Science [cs], [INFO] Computer Science [cs], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience; no abstract
Published: 2011

29. The XMM-Newton Wide-field Survey in the Cosmos Field (XMM-COSMOS): Demography and Multiwavelength Properties of Obscured and Unobscured Luminous Active Galactic Nuclei

Author: Brusa, M., Salvato, M., Capak, P., Zamojski, M., and Scoville, N. Z.
Abstract: We report the final optical identifications of the medium-depth (~60 ks), contiguous (2 deg^2) XMM-Newton survey of the COSMOS field. XMM-Newton has detected ~1800 X-ray sources down to limiting fluxes of ~5 × 10^(–16), ~3 × 10^(–15), and ~7 × 10^(–15) erg cm^(–2) s^(–1) in the 0.5-2 keV, 2-10 keV, and 5-10 keV bands, respectively (~1 × 10^(–15), ~6 × 10^(–15), and ~1 × 10^(–14) erg cm^(–2) s^(–1), in the three bands, respectively, over 50% of the area). The work is complemented by an extensive collection of multiwavelength data from 24 μm to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for ≳50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (~95%) have IRAC counterparts, and 1394 (~78%) have MIPS 24 μm detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of log L_X > 44.5 active galactic nuclei (AGNs) is at z ~ 2. Spectroscopically identified obscured and unobscured AGNs, as well as normal and star-forming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of ~150 high-redshift (z > 1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L_X > 10^(44) erg s^(–1)) X-ray luminosity is ~15%-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations.
Published: 2010

30. Detections of CO Molecular Gas in 24 μm Bright ULIRGs at z ~ 2 in the Spitzer First Look Survey

Author: Yan, Lin, Tacconi, L. J., Fiolet, N., Sajina, A., Omont, A., Lutz, D., Zamojski, M., Neri, R., Cox, P., and Dasyra, K. M.
Abstract: We present CO observations of nine ultra-luminous infrared galaxies (ULIRGs) at z ~ 2 with f_(ν)(24 μm) ≳ 1 mJy, previously confirmed with the mid-IR spectra in the Spitzer First Look Survey. All targets are required to have accurate redshifts from Keck/GEMINI near-IR spectra. Using the Plateau de Bure millimeter-wave Interferometer at the Institute for Radioastronomy at Millimeter Wavelengths, we detect CO J(3-2) (seven objects) or J(2-1) (one object) line emission from eight sources with integrated intensities I_c ~ 5σ-9σ. The CO-detected sources have a variety of mid-IR spectra, including strong polycyclic aromatic hydrocarbon, deep silicate absorption, and power-law continuum, implying that these molecular gas-rich objects at z ~ 2 could be either starbursts or dust-obscured active galactic nuclei (AGNs). The measured line luminosity L'_(CO) is (1.28-3.77) × 10^(10) K km/s pc^2. The averaged molecular gas mass is 1.7 × 10^(10) M_☉, assuming CO-to-H_2 conversion factor of 0.8 M (K km/s pc^2)^(–1). Three sources (33%)—MIPS506, MIPS16144, and MIPS8342—have double peak velocity profiles. The CO double peaks in MIPS506 and MIPS16144 show spatial separations of 45 kpc and 10.9 kpc, allowing the estimates of the dynamical masses of 3.2 × 10^(11) sin^(–2)(i) M_☉ and 5.4 × 10^(11) sin^(–2)(i) M, respectively. The implied gas fraction, M_(gas)/M_(dyn), is 3% and 4%, assuming an average inclination angle. Finally, the analysis of the Hubble Space Telescope/NIC2 images, mid-IR spectra, and IR spectral energy distribution revealed that most of our sources are mergers, containing dust-obscured AGNs dominating the luminosities at (3-6) μm. Together, these results provide some evidence suggesting submillimeter galaxies, bright 24 μm, z ~ 2 ULIRGs, and QSOs could represent three different stages of a single evolutionary sequence, however, a complete physical model would require much more data, especially high spatial resolution spectroscopy.
Published: 2010

31. Molecular gas content in strongly lensedz~ 1.5−3 star-forming galaxies with low infrared luminosities

Author: Dessauges-Zavadsky, M., primary, Zamojski, M., additional, Schaerer, D., additional, Combes, F., additional, Egami, E., additional, Swinbank, A. M., additional, Richard, J., additional, Sklias, P., additional, Rawle, T. D., additional, Rex, M., additional, Kneib, J.-P., additional, Boone, F., additional, and Blain, A., additional
Published: 2015
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32. ALMA detection of [C ii] 158μm emission from a strongly lensedz= 2.013 star-forming galaxy

Author: Schaerer, D., primary, Boone, F., additional, Jones, T., additional, Dessauges-Zavadsky, M., additional, Sklias, P., additional, Zamojski, M., additional, Cava, A., additional, Richard, J., additional, Ellis, R., additional, Rawle, T. D., additional, Egami, E., additional, and Combes, F., additional
Published: 2015
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33. New constraints on dust emission and UV attenuation ofz= 6.5–7.5 galaxies from millimeter observations

Author: Schaerer, D., primary, Boone, F., additional, Zamojski, M., additional, Staguhn, J., additional, Dessauges-Zavadsky, M., additional, Finkelstein, S., additional, and Combes, F., additional
Published: 2015
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34. Galaxy Stellar Mass Assembly between 0.2

Author: Ilbert, O., Salvato, M., Floc'h, E. Le, Aussel, H., Capak, P., McCracken, H. J., Mobasher, B., Kartaltepe, J., Scoville, N., Sanders, D. B., Arnouts, S., Bundy, K., Cassata, P., Kneib, J. -P., Koekemoer, A., Fevre, O. Le, Lilly, S., Surace, J., Taniguchi, Y., Tasca, L., Thompson, D., Tresse, L., Zamojski, M., Zamorani, G., and Zucca, E.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We follow the galaxy stellar mass assembly by morphological and spectral type in the COSMOS 2-deg^2 field. We derive the stellar mass functions and stellar mass densities from z=2 to z=0.2 using 196,000 galaxies selected at F(3.6 micron) > 1 microJy with accurate photometric redshifts (sigma_((zp-zs)/(1+zs))=0.008 at i, 37 pages, 29 figures, accepted for publication in ApJ
Published: 2009
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35. The optical spectra of 24 μm galaxies in the COSMOS field. I. Spitzer MIPS bright sources in the zCOSMOS-bright 10k catalog

Author: Caputi, K. I., Lilly, S. J., Aussel, H., Sanders, D., Frayer, D., Le Fèvre, O., Renzini, A., Zamorani, G., Scodeggio, M., Contini, T., Scoville, N., Carollo, C. M., Hasinger, G., Iovino, A., Le Brun, V., Le Floc'h, E., Maier, C., Mainieri, V., Mignoli, M., Salvato, M., Schiminovich, D., Silverman, J., Surace, J., Tasca, L., Abbas, U., Bardelli, S., Bolzonella, M., Bongiorno, A., Bottini, D., Capak, P., Cappi, A., Cassata, P., Cimatti, A., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Fumana, M., Garilli, B., Halliday, C., Ilbert, O., Kampczyk, P., Kartaltepe, J., Kneib, J.-P., Knobel, C., Kovač, K., Lamareille, F., Leauthaud, A., Le Borgne, J. F., Maccagni, D., Marinoni, C., McCracken, H., Meneux, B., Oesch, P., Pellò, R., Pérez-Montero, E., Porciani, C., Ricciardelli, E., Scaramella, R., Scarlata, C., Tresse, L., Vergani, D., Walcher, J., Zamojski, M., and Zucca, E.
Abstract: We study zCOSMOS-bright optical spectra for 609 Spitzer MIPS 24 μm-selected galaxies with S_(24) μ m > 0.30 mJy and I < 22.5 (AB mag) over 1.5 deg^2 of the COSMOS field. From emission-line diagnostics we find the following: (1) SFRs derived from the observed Hα λ6563 and Hβ λ4861 lines underestimate, on average, the total SFR by factors of ~5 and 10, respectively. (2) Both the Calzetti et al. and the Milky Way reddening laws are suitable to describe the extinction observed in IR sources in most cases. (3) Some IR galaxies at z < 0.3 have low abundances, but many others with similar IR luminosities and redshifts are chemically enriched. (4) The average [O III] λ5007/Hβ λ4861 ratios of ν L^(24 μ m)_ν > 10^(11) Lסּ galaxies at 0.6 < z < 0.7 are ~0.6 dex higher than the average ratio of all zCOSMOS galaxies at similar redshifts. Massive star formation and AGNs could simultaneously be present in those galaxies with the highest ionizing fluxes. (5) Roughly 1/3 of the galaxies with metallicity measurements at 0.5 < z < 0.7 lie below the general mass-metallicity relation at the corresponding redshifts. The strengths of the 4000 Å break and the Hδ EW of our galaxies show that secondary bursts of star formation are needed to explain the spectral properties of most IR sources. The LIRG and ULIRG phases occur, on average, between 10^7 and 10^8 yr after the onset of a starburst on top of underlying older stellar populations. These results are valid for galaxies of different IR luminosities at 0.6 < z < 1.0 and seem independent of the mechanisms triggering star formation.
Published: 2008

36. The optical spectra of 24 mu m galaxies in the cosmos field. I. Spitzer MIPS bright sources in the zCOSMOS-bright 10k catalog

Author: Caputi, K. I., Lilly, S. J., Aussel, H., Sanders, D., Frayer, D., Le Fevre, O., Renzini, A., Zamorani, G., Scodeggio, M., Contini, T., Scoville, N., Carollo, C. M., Hasinger, G., Iovino, A., Le Brun, V., Le Floc'h, E., Maier, C., Mainieri, V., Mignoli, M., Salvato, M., Schiminovich, D., Silverman, J., Surace, J., Tasca, L., Abbas, U., Bardelli, S., Bolzonella, M., Bongiorno, A., Bottini, D., Capak, P., Cappi, A., Cassata, P., Cimatti, A., Cucciati, O., de la Torre, S., de Ravel, L., Franzetti, P., Fumana, M., Garilli, B., Halliday, C., Ilbert, O., Kampczyk, P., Kartaltepe, J., Kneib, J. -P., Knobel, C., Kovac, K., Lamareille, F., Leauthaud, A., Le Borgne, J. F., Maccagni, D., Marinoni, C., McCracken, H., Meneux, B., Oesch, P., Pello, R., Perez-Montero, E., Porciani, C., Ricciardelli, E., Scaramella, R., Scarlata, C., Tresse, L., Vergani, D., Walcher, J., Zamojski, M., Zucca, E., and Astronomy
Subjects: ACTIVE GALACTIC NUCLEI, galaxies : evolution, infrared : galaxies, FRANCE REDSHIFT SURVEY, galaxies : active, MASS-METALLICITY RELATION, ENERGY-DISTRIBUTIONS, LUMINOUS INFRARED GALAXIES, EMISSION-LINE SPECTRA, MU-M SOURCES, STAR-FORMING GALAXIES, DIGITAL SKY SURVEY, SPACE-TELESCOPE, galaxies : abundances
Abstract: We study zCOSMOS-bright optical spectra for 609 Spitzer MIPS 24 mu m-selected galaxies with S-24 (mu m) > 0: 30 mJy and I 10(11) L-circle dot galaxies at 0.6
Published: 2008

37. [C II] AND12CO(1-0) EMISSION MAPS IN HLSJ091828.6+514223: A STRONGLY LENSED INTERACTING SYSTEM ATz= 5.24

Author: Rawle, T. D., primary, Egami, E., additional, Bussmann, R. S., additional, Gurwell, M., additional, Ivison, R. J., additional, Boone, F., additional, Combes, F., additional, Danielson, A. L. R., additional, Rex, M., additional, Richard, J., additional, Smail, I., additional, Swinbank, A. M., additional, Altieri, B., additional, Blain, A. W., additional, Clement, B., additional, Dessauges-Zavadsky, M., additional, Edge, A. C., additional, Fazio, G. G., additional, Jones, T., additional, Kneib, J.-P., additional, Omont, A., additional, Pérez-González, P. G., additional, Schaerer, D., additional, Valtchanov, I., additional, van der Werf, P. P., additional, Walth, G., additional, Zamojski, M., additional, and Zemcov, M., additional
Published: 2014
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38. Star formation histories, extinction, and dust properties of strongly lensedz~ 1.5–3 star-forming galaxies from theHerschelLensing Survey

Author: Sklias, P., primary, Zamojski, M., additional, Schaerer, D., additional, Dessauges-Zavadsky, M., additional, Egami, E., additional, Rex, M., additional, Rawle, T., additional, Richard, J., additional, Boone, F., additional, Simpson, J. M., additional, Smail, I., additional, van der Werf, P., additional, Altieri, B., additional, and Kneib, J. P., additional
Published: 2014
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39. Photometry in UV astronomical images of extended sources in crowded field using deblended images in optical visible bands as Bayesian priors

Author: Bouman, Charles A., Miller, Eric L., Pollak, Ilya, Vibert, D., Zamojski, M., Conseil, S., Llebaria, A., Arnouts, S., Milliard, B., Guillaume, M., Bouman, Charles A., Miller, Eric L., Pollak, Ilya, Vibert, D., Zamojski, M., Conseil, S., Llebaria, A., Arnouts, S., Milliard, B., and Guillaume, M.
Abstract: Photometry of astrophysical sources, galaxies and stars, in crowded field images, if an old problem, is still a challenging goal, as new space survey missions are launched, releasing new data with increased sensibility, resolution and field of view. The GALEX mission, observes in two UV bands and produces deep sky images of millions of galaxies or stars mixed together. These UV observations are of lower resolution than same field observed in visible bands, and with a very faint signal, at the level of the photon noise for a substantial fraction of objects. Our purpose is to use the better known optical counterparts as prior information in a Bayesian approach to deduce the UV flux. Photometry of extended sources has been addressed several times using various techniques: background determination via sigma clipping, adaptative-aperture, point-spread-function photometry, isophotal photometry, to lists some. The Bayesian approach of using optical priors for solving the UV photometry has already been applied by our team in a previous work. Here we describe the improvement of using the extended shape inferred by deblending the high resolution optical images and not only the position of the optical sources. The resulting photometric accuracy has been tested with simulation of crowded UV fields added on top of real UV images. Finally, this helps to converge to smaller and flat residual and increase the faint source detection threshold. It thus gives the opportunity to work on 2nd order effects, like improving the knowledge of the background or point-spread function by iterating on them.
Published: 2009

40. An extendedHerscheldrop-out source in the center of AS1063: a normal dusty galaxy atz= 6.1 or SZ substructures?

Author: Boone, F., primary, Clément, B., additional, Richard, J., additional, Schaerer, D., additional, Lutz, D., additional, Weiß, A., additional, Zemcov, M., additional, Egami, E., additional, Rawle, T. D., additional, Walth, G. L., additional, Kneib, J.-P., additional, Combes, F., additional, Smail, I., additional, Swinbank, A. M., additional, Altieri, B., additional, Blain, A. W., additional, Chapman, S., additional, Dessauges-Zavadsky, M., additional, Ivison, R. J., additional, Knudsen, K. K., additional, Omont, A., additional, Pelló, R., additional, Pérez-González, P. G., additional, Valtchanov, I., additional, van der Werf, P., additional, and Zamojski, M., additional
Published: 2013
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41. SPECTRAL ENERGY DISTRIBUTIONS OF TYPE 1 ACTIVE GALACTIC NUCLEI IN THE COSMOS SURVEY. I. THEXMM-COSMOS SAMPLE

Author: Elvis, M., primary, Hao, H., additional, Civano, F., additional, Brusa, M., additional, Salvato, M., additional, Bongiorno, A., additional, Capak, P., additional, Zamorani, G., additional, Comastri, A., additional, Jahnke, K., additional, Lusso, E., additional, Mainieri, V., additional, Trump, J. R., additional, Ho, L. C., additional, Aussel, H., additional, Cappelluti, N., additional, Cisternas, M., additional, Frayer, D., additional, Gilli, R., additional, Hasinger, G., additional, Huchra, J. P., additional, Impey, C. D., additional, Koekemoer, A. M., additional, Lanzuisi, G., additional, Le Floc'h, E., additional, Lilly, S. J., additional, Liu, Y., additional, McCarthy, P., additional, McCracken, H. J., additional, Merloni, A., additional, Roeser, H.-J., additional, Sanders, D. B., additional, Sargent, M., additional, Scoville, N., additional, Schinnerer, E., additional, Schiminovich, D., additional, Silverman, J., additional, Taniguchi, Y., additional, Vignali, C., additional, Urry, C. M., additional, Zamojski, M. A., additional, and Zatloukal, M., additional
Published: 2012
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42. Far-infrared constraints on the contamination by dust-obscured galaxies of high-zdropout searches

Author: Boone, F., primary, Schaerer, D., additional, Pelló, R., additional, Lutz, D., additional, Weiss, A., additional, Egami, E., additional, Smail, I., additional, Rex, M., additional, Rawle, T., additional, Ivison, R., additional, Laporte, N., additional, Beelen, A., additional, Combes, F., additional, Blain, A. W., additional, Richard, J., additional, Kneib, J.-P., additional, Zamojski, M., additional, Dessauges-Zavadsky, M., additional, Altieri, B., additional, van der Werf, P., additional, Swinbank, M., additional, Pérez-González, P. G., additional, Clement, B., additional, Nordon, R., additional, Magnelli, B., additional, and Menten, K. M., additional
Published: 2011
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43. THEXMM-NEWTONWIDE-FIELD SURVEY IN THE COSMOS FIELD (XMM-COSMOS): DEMOGRAPHY AND MULTIWAVELENGTH PROPERTIES OF OBSCURED AND UNOBSCURED LUMINOUS ACTIVE GALACTIC NUCLEI

Author: Brusa, M., primary, Civano, F., additional, Comastri, A., additional, Miyaji, T., additional, Salvato, M., additional, Zamorani, G., additional, Cappelluti, N., additional, Fiore, F., additional, Hasinger, G., additional, Mainieri, V., additional, Merloni, A., additional, Bongiorno, A., additional, Capak, P., additional, Elvis, M., additional, Gilli, R., additional, Hao, H., additional, Jahnke, K., additional, Koekemoer, A. M., additional, Ilbert, O., additional, Le Floc'h, E., additional, Lusso, E., additional, Mignoli, M., additional, Schinnerer, E., additional, Silverman, J. D., additional, Treister, E., additional, Trump, J. D., additional, Vignali, C., additional, Zamojski, M., additional, Aldcroft, T., additional, Aussel, H., additional, Bardelli, S., additional, Bolzonella, M., additional, Cappi, A., additional, Caputi, K., additional, Contini, T., additional, Finoguenov, A., additional, Fruscione, A., additional, Garilli, B., additional, Impey, C. D., additional, Iovino, A., additional, Iwasawa, K., additional, Kampczyk, P., additional, Kartaltepe, J., additional, Kneib, J. P., additional, Knobel, C., additional, Kovac, K., additional, Lamareille, F., additional, Leborgne, J.-F., additional, Le Brun, V., additional, Le Fevre, O., additional, Lilly, S. J., additional, Maier, C., additional, McCracken, H. J., additional, Pello, R., additional, Peng, Y.-J., additional, Perez-Montero, E., additional, de Ravel, L., additional, Sanders, D., additional, Scodeggio, M., additional, Scoville, N. Z., additional, Tanaka, M., additional, Taniguchi, Y., additional, Tasca, L., additional, de la Torre, S., additional, Tresse, L., additional, Vergani, D., additional, and Zucca, E., additional
Published: 2010
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44. DETECTIONS OF CO MOLECULAR GAS IN 24 μm BRIGHT ULIRGs ATz∼ 2 IN THESPITZERFIRST LOOK SURVEY

Author: Yan, Lin, primary, Tacconi, L. J., additional, Fiolet, N., additional, Sajina, A., additional, Omont, A., additional, Lutz, D., additional, Zamojski, M., additional, Neri, R., additional, Cox, P., additional, and Dasyra, K. M., additional
Published: 2010
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45. GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 < 2 FROM THE S-COSMOS SURVEY

Author: Ilbert, O., primary, Salvato, M., additional, Le Floc'h, E., additional, Aussel, H., additional, Capak, P., additional, McCracken, H. J., additional, Mobasher, B., additional, Kartaltepe, J., additional, Scoville, N., additional, Sanders, D. B., additional, Arnouts, S., additional, Bundy, K., additional, Cassata, P., additional, Kneib, J.-P., additional, Koekemoer, A., additional, Le Fèvre, O., additional, Lilly, S., additional, Surace, J., additional, Taniguchi, Y., additional, Tasca, L., additional, Thompson, D., additional, Tresse, L., additional, Zamojski, M., additional, Zamorani, G., additional, and Zucca, E., additional
Published: 2010
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46. THE OPTICAL SPECTRA OFSPITZER24 μm GALAXIES IN THE COSMIC EVOLUTION SURVEY FIELD. II. FAINT INFRARED SOURCES IN THE zCOSMOS-BRIGHT 10k CATALOG

Author: Caputi, K. I., primary, Lilly, S. J., additional, Aussel, H., additional, Floc'h, E. Le, additional, Sanders, D., additional, Maier, C., additional, Frayer, D., additional, Carollo, C. M., additional, Contini, T., additional, Kneib, J.-P., additional, Le Fèvre, O., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, Scoville, N., additional, Zamorani, G., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Ilbert, O., additional, Iovino, A., additional, Kampczyk, P., additional, Kartaltepe, J., additional, Knobel, C., additional, Kovač, K., additional, Lamareille, F., additional, Le Borgne, J.-F., additional, Le Brun, V., additional, Mignoli, M., additional, Peng, Y., additional, Pérez-Montero, E., additional, Ricciardelli, E., additional, Salvato, M., additional, Silverman, J., additional, Surace, J., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, Zucca, E., additional, Abbas, U., additional, Bottini, D., additional, Capak, P., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Elvis, M., additional, Hasinger, G., additional, Koekemoer, A. M., additional, Leauthaud, A., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H., additional, Memeo, P., additional, Meneux, B., additional, Oesch, P., additional, Pellò, R., additional, Porciani, C., additional, Pozzetti, L., additional, Scaramella, R., additional, Scarlata, C., additional, Schiminovich, D., additional, Taniguchi, Y., additional, and Zamojski, M., additional
Published: 2009
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47. Photometry in UV astronomical images of extended sources in crowded field using deblended images in optical visible bands as Bayesian priors

Author: Vibert, D., primary, Zamojski, M., additional, Conseil, S., additional, Llebaria, A., additional, Arnouts, S., additional, Milliard, B., additional, and Guillaume, M., additional
Published: 2009
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48. PHOTOMETRIC REDSHIFT AND CLASSIFICATION FOR THEXMM-COSMOS SOURCES

Author: Salvato, M., primary, Hasinger, G., additional, Ilbert, O., additional, Zamorani, G., additional, Brusa, M., additional, Scoville, N. Z., additional, Rau, A., additional, Capak, P., additional, Arnouts, S., additional, Aussel, H., additional, Bolzonella, M., additional, Buongiorno, A., additional, Cappelluti, N., additional, Caputi, K., additional, Civano, F., additional, Cook, R., additional, Elvis, M., additional, Gilli, R., additional, Jahnke, K., additional, Kartaltepe, J. S., additional, Impey, C. D., additional, Lamareille, F., additional, Le Floch, E., additional, Lilly, S., additional, Mainieri, V., additional, McCarthy, P., additional, McCracken, H., additional, Mignoli, M., additional, Mobasher, B., additional, Murayama, T., additional, Sasaki, S., additional, Sanders, D. B., additional, Schiminovich, D., additional, Shioya, Y., additional, Shopbell, P., additional, Silverman, J., additional, Smolčić, V., additional, Surace, J., additional, Taniguchi, Y., additional, Thompson, D., additional, Trump, J. R., additional, Urry, M., additional, and Zamojski, M., additional
Published: 2008
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49. COSMOS PHOTOMETRIC REDSHIFTS WITH 30-BANDS FOR 2-deg2

Author: Ilbert, O., primary, Capak, P., additional, Salvato, M., additional, Aussel, H., additional, McCracken, H. J., additional, Sanders, D. B., additional, Scoville, N., additional, Kartaltepe, J., additional, Arnouts, S., additional, Floc'h, E. Le, additional, Mobasher, B., additional, Taniguchi, Y., additional, Lamareille, F., additional, Leauthaud, A., additional, Sasaki, S., additional, Thompson, D., additional, Zamojski, M., additional, Zamorani, G., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Brusa, M., additional, Caputi, K. I., additional, Carollo, C. M., additional, Contini, T., additional, Cook, R., additional, Coppa, G., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Garilli, B., additional, Hasinger, G., additional, Iovino, A., additional, Kampczyk, P., additional, Kneib, J.-P., additional, Knobel, C., additional, Kovac, K., additional, Le Borgne, J. F., additional, Le Brun, V., additional, Fèvre, O. Le, additional, Lilly, S., additional, Looper, D., additional, Maier, C., additional, Mainieri, V., additional, Mellier, Y., additional, Mignoli, M., additional, Murayama, T., additional, Pellò, R., additional, Peng, Y., additional, Pérez-Montero, E., additional, Renzini, A., additional, Ricciardelli, E., additional, Schiminovich, D., additional, Scodeggio, M., additional, Shioya, Y., additional, Silverman, J., additional, Surace, J., additional, Tanaka, M., additional, Tasca, L., additional, Tresse, L., additional, Vergani, D., additional, and Zucca, E., additional
Published: 2008
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50. The Optical Spectra of 24 μm Galaxies in the COSMOS Field. I.SpitzerMIPS Bright Sources in the zCOSMOS‐Bright 10k Catalog

Author: Caputi, K. I., primary, Lilly, S. J., additional, Aussel, H., additional, Sanders, D., additional, Frayer, D., additional, Le Fèvre, O., additional, Renzini, A., additional, Zamorani, G., additional, Scodeggio, M., additional, Contini, T., additional, Scoville, N., additional, Carollo, C. M., additional, Hasinger, G., additional, Iovino, A., additional, Le Brun, V., additional, Le Floc’h, E., additional, Maier, C., additional, Mainieri, V., additional, Mignoli, M., additional, Salvato, M., additional, Schiminovich, D., additional, Silverman, J., additional, Surace, J., additional, Tasca, L., additional, Abbas, U., additional, Bardelli, S., additional, Bolzonella, M., additional, Bongiorno, A., additional, Bottini, D., additional, Capak, P., additional, Cappi, A., additional, Cassata, P., additional, Cimatti, A., additional, Cucciati, O., additional, de la Torre, S., additional, de Ravel, L., additional, Franzetti, P., additional, Fumana, M., additional, Garilli, B., additional, Halliday, C., additional, Ilbert, O., additional, Kampczyk, P., additional, Kartaltepe, J., additional, Kneib, J.‐P., additional, Knobel, C., additional, Kovac, K., additional, Lamareille, F., additional, Leauthaud, A., additional, Le Borgne, J. F., additional, Maccagni, D., additional, Marinoni, C., additional, McCracken, H., additional, Meneux, B., additional, Oesch, P., additional, Pellò, R., additional, Pérez‐Montero, E., additional, Porciani, C., additional, Ricciardelli, E., additional, Scaramella, R., additional, Scarlata, C., additional, Tresse, L., additional, Vergani, D., additional, Walcher, J., additional, Zamojski, M., additional, and Zucca, E., additional
Published: 2008
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