RT Journal Article
T1 The relation between cool cluster cores and Herschel-detected star formation in brightest cluster galaxies
A1 Pérez González, Pablo Guillermo
A1 otros, ...
AB We present far-infrared (FIR) analysis of 68 brightest cluster galaxies (BCGs) at 0.08 < z < 1.0. Deriving total infrared luminosities directly from Spitzer and Herschel photometry spanning the peak of the dust component (24-500 μm), we calculate the obscured star formation rate (SFR). 22^+6.2 _–5.3% of the BCGs are detected in the far-infrared, with SFR = 1-150 M ☉ yr^–1. The infrared luminosity is highly correlated with cluster X-ray gas cooling times for cool-core clusters (gas cooling time <1 Gyr), strongly suggesting that the star formation in these BCGs is influenced by the cluster-scale cooling process. The occurrence of the molecular gas tracing Hα emission is also correlated with obscured star formation. For all but the most luminous BCGs (L_TIR > 2 × 10^11 L_☉), only a small (≤0.4 mag) reddening correction is required for SFR(Hα) to agree with SFR_FIR. The relatively low Hα extinction (dust obscuration), compared to values reported for the general star-forming population, lends further weight to an alternate (external) origin for the cold gas. Finally, we use a stacking analysis of non-cool-core clusters to show that the majority of the fuel for star formation in the FIR-bright BCGs is unlikely to originate from normal stellar mass loss.
PB American Astronomical Society
SN 0004-637X
YR 2012
FD 2012-03-01
LK https://hdl.handle.net/20.500.14352/45095
UL https://hdl.handle.net/20.500.14352/45095
LA eng
NO Adelman-McCarthy, J. K., Agüeros, M. A., Allam, S. S., et al. 2008, ApJS, 175, 297Arnouts, S., Walcher, C. J., Le Fèvre, O., et al. 2007, A&A, 476, 137Berta, S., Magnelli, B., Lutz, D., et al. 2010, A&A, 518, L30Bertin, E., & Arnouts, S. 1996, A&A, 117, 393Bildfell, C., Hoekstra, H., Babul, A., et al. 2008, MNRAS, 389, 1637Blain, A. W., Barnard, V. E., & Chapman, S. C. 2003, MNRAS, 338, 733Böhringer, H., Voges, W., Fabian, A. C., Edge, A. C., & Neumann, D. M. 1993, MNRAS, 264, 25Bower, R. G., Benson, A. J., Malbon, R., et al. 2006, MNRAS, 370, 645Calzetti, D., Wu, S.-Y., Hong, S., et al. 2010, ApJ, 714, 1256Cavagnolo, K. W., Donahue, M., Voit, G. M., & Sun, M. 2008, ApJ, 683, 107Cavagnolo, K. W., Donahue, M., Voit, G. M., & Sun, M. 2009, ApJS, 182, 12Chary, R., & Elbaz, D. 2001, ApJ, 556, 562Conselice, C. S., Gallagher, J. S., & Wyse, R. F. G. 2001, AJ, 122, 2281Cowie, L. L., & Binney, J. 1977, ApJ, 215, 723Crawford, C. S., Allen, S. W., Ebeling, H., Edge, A. C., & Fabian, A. C. 1999, MNRAS, 306, 857Crawford, C. S., Hatch, N. A., Fabian, A. C., & Sanders, J. S. 2005, MNRAS, 363, 216Dale, D. A., & Helou, G. 2002, ApJ, 576, 159David, L. P., & Kempner, J. 2004, ApJ, 613, 831Donahue, M., de Messières, G. E., O’Connell, R. W., et al. 2011, ApJ, 732, 40Donahue, M., Stocke, J. T., & Gioia, I. M. 1992, ApJ, 385, 49Donahue, M., Voit, G. M., O’Dea, C. P., Baum, S. A., & Sparks, W. B. 2005, ApJ, 630, L13Draine, B. T. 2003, ARA&A, 41, 241Edge, A. C. 2001, MNRAS, 328, 762Edge, A. C., Stewart, G. C., & Fabian, A. C. 1992, MNRAS, 258, 177Edge, A. C., Oonk, J. B. R., Mittal, R., et al. 2010a, A&A, 518, L46Edge, A. C., Oonk, J. B. R., Mittal, R., et al. 2010b, A&A, 518, L47 (E10)Edge, A. C., Wilman, R. J., Johnstone, R. M., et al. 2002, MNRAS, 337, 49Egami, E., Misselt, K. A., Rieke, G. H., et al. 2006a, ApJ, 647, 922Egami, E., Rex, M., Rawle, T. D., et al. 2010, A&A, 518, L12Egami, E., Rieke, G. H., Fadda, D., & Hines, D. C. 2006b, ApJ, 652, L21Fabian, A. C., & Nulsen, P. E. J. 1977, MNRAS, 180, 479Fabian, A. C., Sanders, J. S., Williams, R. J. R., et al. 2011, MNRAS, 417, 172Griffin, M., Abergel, A., Abreu, A., et al. 2010, A&A, 518, L3Haines, C. P., Smith, G. P., Egami, E., et al. 2009, ApJ, 704, 126Hopkins, A. M., Connolly, A. J., Haarsma, D. B., et al. 2001, AJ, 122, 288Hudson, D. S., Mittal, R., Reiprich, T. H., et al. 2010, A&A, 513, 37Hwang, H. S., Elbaz, D., Magdis, G., et al. 2010, MNRAS, 409, 75Johnstone, R. M., Hatch, N. A., Ferland, G. J., et al. 2007, MNRAS, 382, 1246Kennicutt, R. C., Jr. 1983, ApJ, 272, 54Kennicutt, R. C., Jr. 1998, ARA&A, 36, 189Marsden, G., Ade, P. A. R., Bock, J. J., et al. 2009, ApJ, 707, 1729McDonald, M., Veilleux, S., & Mushotzky, R. 2011, ApJ, 731, 33McNamara, B. R., & Nulsen, P. E. J. 2007, ARA&A, 45, 117McNamara, B. R., Wise, M., Nulsen, P. E. J., et al. 2000, ApJ, 534, 135Mittal, R., O’Dea, C. P., Ferland, G., et al. 2011, MNRAS, 418, 2386Nguyen, H. T., Schulz, B., Levenson, L., et al. 2010, A&A, 518, L5O’Dea, C. P., Baum, S. A., Privon, G., et al. 2008, ApJ, 681, 1035Okabe, N., Takada, M., Umetsu, K., Futamase, T., & Smith, G. P. 2010, PASJ, 62, 811Ott, S. 2010, in ASP Conf. Ser. 434, Astronomical Data Analysis Software and Systems XIX, ed. Y. Mizumoto, K.-I. Morita, & M. Ohishi (San Francisco, CA: ASP), 139Peterson, J. R., & Fabian, A. C. 2006, Phys. Rep., 427, 1Pilbratt, G., Riedinger, J. R., Passvogel, T., et al. 2010, A&A, 518, L1Poglitsch, A., Waelkens, C., Geis, N., et al. 2010, A&A, 518, L2Quillen, A. C., Zufelt, N., Park, J., et al. 2008, ApJS, 176, 39Rawle, T. D., Chung, S. M., Fadda, D., et al. 2010, A&A, 518, L14Rex, M., Rawle, T. D., Egami, E., et al. 2010, A&A, 518, L13Rieke, G. H., Alonso Herrero, A., Weiner, B. J., et al. 2009, ApJ, 692, 556 (R09)Salomé, P., & Combes, F. 2003, A&A, 412, 657Silk, J., & Rees, M. J. 1998, A&A, 331, 1Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163Smith, G., Haines, C. P., Pereira, M. J., et al. 2010, A&A, 518, L18Tamura, T., Kaastra, J. S., Peterson, J. R., et al. 2001, A&A, 365, L87Voit, G. M., & Donahue, M. 2011, ApJ, 738, L24Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, AJ, 140, 1868
NO © 2012 The American Astronomical Society.Artículo firmado por 15 autores. This work is partially based on observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We also thank the HSC and NHSC consortia for support with data reduction. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. G. P. S. acknowledges support from the Royal Society.
NO National Aeronautics and Space Administration (NASA)
NO JPL/Caltech (NASA)
NO National Science Foundation (NSF)
NO Royal Society
DS Docta Complutense
RD 9 may 2024