Search

Your search keyword '"Sargent M."' showing total 31 results
Start Over Author "Sargent M." Journal monthly notices of the royal astronomical society
31 results on '"Sargent M."'

1. SKA science data challenge 2: analysis and results

Author

Hartley, P, primary, Bonaldi, A, additional, Braun, R, additional, Aditya, J N H S, additional, Aicardi, S, additional, Alegre, L, additional, Chakraborty, A, additional, Chen, X, additional, Choudhuri, S, additional, Clarke, A O, additional, Coles, J, additional, Collinson, J S, additional, Cornu, D, additional, Darriba, L, additional, Veneri, M Delli, additional, Forbrich, J, additional, Fraga, B, additional, Galan, A, additional, Garrido, J, additional, Gubanov, F, additional, Håkansson, H, additional, Hardcastle, M J, additional, Heneka, C, additional, Herranz, D, additional, Hess, K M, additional, Jagannath, M, additional, Jaiswal, S, additional, Jurek, R J, additional, Korber, D, additional, Kitaeff, S, additional, Kleiner, D, additional, Lao, B, additional, Lu, X, additional, Mazumder, A, additional, Moldón, J, additional, Mondal, R, additional, Ni, S, additional, Önnheim, M, additional, Parra, M, additional, Patra, N, additional, Peel, A, additional, Salomé, P, additional, Sánchez-Expósito, S, additional, Sargent, M, additional, Semelin, B, additional, Serra, P, additional, Shaw, A K, additional, Shen, A X, additional, Sjöberg, A, additional, Smith, L, additional, Soroka, A, additional, Stolyarov, V, additional, Tolley, E, additional, Toribio, M C, additional, van der Hulst, J M, additional, Sadr, A Vafaei, additional, Verdes-Montenegro, L, additional, Westmeier, T, additional, Yu, K, additional, Yu, L, additional, Zhang, L, additional, Zhang, X, additional, Zhang, Y, additional, Alberdi, A, additional, Ashdown, M, additional, Bom, C R, additional, Brüggen, M, additional, Cannon, J, additional, Chen, R, additional, Combes, F, additional, Conway, J, additional, Courbin, F, additional, Ding, J, additional, Fourestey, G, additional, Freundlich, J, additional, Gao, L, additional, Gheller, C, additional, Guo, Q, additional, Gustavsson, E, additional, Jirstrand, M, additional, Jones, M G, additional, Józsa, G, additional, Kamphuis, P, additional, Kneib, J-P, additional, Lindqvist, M, additional, Liu, B, additional, Liu, Y, additional, Mao, Y, additional, Marchal, A, additional, Márquez, I, additional, Meshcheryakov, A, additional, Olberg, M, additional, Oozeer, N, additional, Pandey-Pommier, M, additional, Pei, W, additional, Peng, B, additional, Sabater, J, additional, Sorgho, A, additional, Starck, J L, additional, Tasse, C, additional, Wang, A, additional, Wang, Y, additional, Xi, H, additional, Yang, X, additional, Zhang, H, additional, Zhang, J, additional, Zhao, M, additional, and Zuo, S, additional

Published
2023
Full Text
View/download PDF

2. Dust grain size evolution in local galaxies: a comparison between observations and simulations

Author

Relaño, M, primary, De Looze, I, additional, Saintonge, A, additional, Hou, K-C, additional, Romano, L E C, additional, Nagamine, K, additional, Hirashita, H, additional, Aoyama, S, additional, Lamperti, I, additional, Lisenfeld, U, additional, Smith, M W L, additional, Chastenet, J, additional, Xiao, T, additional, Gao, Y, additional, Sargent, M, additional, and van der Giessen, S A, additional

Published
2022
Full Text
View/download PDF

3. The Herschel* PEP-HERMES Luminosity Function- I. Probing the Evolution of PACS Selected Galaxies to z approx. equal to 4

Author

Gruppioni, Carlotta, Pozzi, F, Rodighiero, G, Delvecchio, I, Berta, S, Pozzetti, L, Zamorani, G, Andreani, P, Cimatti, A, Ilbert, O, LeFloc'h, E, Lutz, D, Magnelli, B, Marchetti, L, Monaco, P, Nordon, R, Oliver, S, Popesso, P, Riguccini, L, Roseboom, I, Rosario, D. J, Sargent, M, Vaccari, M, Altieri, B, Amblard, A, Bock, J, Dowell, C. D, Dwek, E, Levenson, L, Lu, N, Nguyen, H. T, Schulz, B, Shupe, D. L, and Xu, C. K

Subjects
Astrophysics, Astronomy
Abstract

We exploit the deep and extended far-IR data sets (at 70, 100 and 160 μm) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 μm, to derive the evolution of the rest-frame 35-, 60-, 90- and total infrared (IR) luminosity functions (LFs) up to z ∼ 4.We detect very strong luminosity evolution for the total IR LF (LIR ∝ (1 + z)(sup 3.55 +/- 0.10) up to z ∼ 2, and ∝ (1 + z)(sup 1.62 +/- 0.51) at 2 less than z less than approximately 4) combined with a density evolution (∝ (1 + z)(sup −0.57 +/- 0.22) up to z ∼ 1 and ∝ (1 + z)(sup −3.92 +/- 0.34) at 1 less than z less than approximately 4). In agreement with previous findings, the IR luminosity density (ρIR) increases steeply to z ∼ 1, then flattens between z ∼ 1 and z ∼ 3 to decrease at z greater than approximately 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to ρIR. Galaxies occupying the well-established SFR-stellar mass main sequence (MS) are found to dominate both the total IR LF and ρIR at all redshifts, with the contribution from off-MS sources (≥0.6 dex above MS) being nearly constant (∼20 per cent of the total ρIR) and showing no significant signs of increase with increasing z over the whole 0.8 < z <2.2 range. Sources with mass in the range 10 ≤ log(M/solar mass) ≤ 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (greater than approximately 2) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies.

Published
2013
Full Text
View/download PDF

5. JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

Author

De Looze, I, primary, Lamperti, I, primary, Saintonge, A, primary, Relaño, M, primary, Smith, M W L, primary, Clark, C J R, primary, Wilson, C D, primary, Decleir, M, primary, Jones, A P, primary, Kennicutt, R C, primary, Accurso, G, primary, Brinks, E, primary, Bureau, M, primary, Cigan, P, primary, Clements, D L, primary, De Vis, P, primary, Fanciullo, L, primary, Gao, Y, primary, Gear, W K, primary, Ho, L C, primary, Hwang, H S, primary, Michałowski, M J, primary, Lee, J C, primary, Li, C, primary, Lin, L, primary, Liu, T, primary, Lomaeva, M, primary, Pan, H-A, primary, Sargent, M, primary, Williams, T, primary, Xiao, T, primary, and Zhu, M, primary

Published
2020
Full Text
View/download PDF

6. The e-MERGE Survey (e-MERLIN Galaxy Evolution Survey): overview and survey description

Author

Muxlow, T W B, primary, Thomson, A P, additional, Radcliffe, J F, additional, Wrigley, N H, additional, Beswick, R J, additional, Smail, Ian, additional, McHardy, I M, additional, Garrington, S T, additional, Ivison, R J, additional, Jarvis, M J, additional, Prandoni, I, additional, Bondi, M, additional, Guidetti, D, additional, Argo, M K, additional, Bacon, David, additional, Best, P N, additional, Biggs, A D, additional, Chapman, S C, additional, Coppin, K, additional, Chen, H, additional, Garratt, T K, additional, Garrett, M A, additional, Ibar, E, additional, Kneib, Jean-Paul, additional, Knudsen, Kirsten K, additional, Koopmans, L V E, additional, Morabito, L K, additional, Murphy, E J, additional, Njeri, A, additional, Pearson, Chris, additional, Pérez-Torres, M A, additional, Richards, A M S, additional, Röttgering, H J A, additional, Sargent, M T, additional, Serjeant, Stephen, additional, Simpson, C, additional, Simpson, J M, additional, Swinbank, A M, additional, Varenius, E, additional, and Venturi, T, additional

Published
2020
Full Text
View/download PDF

10. A3COSMOS: the dust attenuation of star-forming galaxies at z = 2.5–4.0 from the COSMOS-ALMA archive.

Author

Fudamoto, Yoshinobu, Oesch, P A, Magnelli, B, Schinnerer, E, Liu, D, Lang, P, Jiménez-Andrade, E F, Groves, B, Leslie, S, and Sargent, M T

Subjects
DUST, STELLAR mass, STARBURSTS, GALAXIES, GALACTIC evolution, GALAXY formation
Abstract

We present an analysis of the dust attenuation of star-forming galaxies at z  = 2.5–4.0 through the relationship between the UV spectral slope (β), stellar mass (M *), and the infrared excess (IRX = L IR/ L UV) based on far-infrared continuum observations from the Atacama Large Millimeter/sub-millimeter Array (ALMA). Our study exploits the full ALMA archive over the COSMOS field processed by the A3COSMOS team, which includes an unprecedented sample of ∼1500 galaxies at z ∼ 3 as primary or secondary targets in ALMA band 6 or 7 observations with a median continuum sensitivity of 126 |$\rm {\mu Jy\, beam}^{-1}$| (1σ). The detection rate is highly mass dependent, decreasing drastically below log (M */M⊙) = 10.5. The detected galaxies show that the IRX–β relationship of massive (log  M */M⊙ > 10) main-sequence galaxies at z  = 2.5–4.0 is consistent with that of local galaxies, while starbursts are generally offset by |$\sim 0.5\, {\rm dex}$| to larger IRX values. At the low-mass end, we derive upper limits on the infrared luminosities through stacking of the ALMA data. The combined IRX– M * relation at |$\rm {log\, ({\it M}_{\ast }/\mathrm{M}_{\odot })\gt 9}$| exhibits a significantly steeper slope than reported in previous studies at similar redshifts, implying little dust obscuration at log  M */M⊙ < 10. However, our results are consistent with earlier measurements at z ∼ 5.5, indicating a potential redshift evolution between z ∼ 2 and z ∼ 6. Deeper observations targeting low-mass galaxies will be required to confirm this finding. [ABSTRACT FROM AUTHOR]

Published
2020
Full Text
View/download PDF

12. The [C ii] emission as a molecular gas mass tracer in galaxies at low and high redshifts

Author

Zanella, A, primary, Daddi, E, additional, Magdis, G, additional, Diaz Santos, T, additional, Cormier, D, additional, Liu, D, additional, Cibinel, A, additional, Gobat, R, additional, Dickinson, M, additional, Sargent, M, additional, Popping, G, additional, Madden, S C, additional, Bethermin, M, additional, Hughes, T M, additional, Valentino, F, additional, Rujopakarn, W, additional, Pannella, M, additional, Bournaud, F, additional, Walter, F, additional, Wang, T, additional, Elbaz, D, additional, and Coogan, R T, additional

Published
2018
Full Text
View/download PDF

13. Merger driven star-formation activity in Cl J1449+0856 at z=1.99 as seen by ALMA and JVLA

Author

Coogan, R T, primary, Daddi, E, additional, Sargent, M T, additional, Strazzullo, V, additional, Valentino, F, additional, Gobat, R, additional, Magdis, G, additional, Bethermin, M, additional, Pannella, M, additional, Onodera, M, additional, Liu, D, additional, Cimatti, A, additional, Dannerbauer, H, additional, Carollo, M, additional, Renzini, A, additional, and Tremou, E, additional

Published
2018
Full Text
View/download PDF

14. Red, redder, reddest: SCUBA-2 imaging of colour-selected Herschel sources

Author

Duivenvoorden, S, primary, Oliver, S, additional, Scudder, J M, additional, Greenslade, J, additional, Riechers, D A, additional, Wilkins, S M, additional, Buat, V, additional, Chapman, S C, additional, Clements, D L, additional, Cooray, A, additional, Coppin, K E K, additional, Dannerbauer, H, additional, De Zotti, G, additional, Dunlop, J S, additional, Eales, S A, additional, Efstathiou, A, additional, Farrah, D, additional, Geach, J E, additional, Holland, W S, additional, Hurley, P D, additional, Ivison, R J, additional, Marchetti, L, additional, Petitpas, G, additional, Sargent, M T, additional, Scott, D, additional, Symeonidis, M, additional, Vaccari, M, additional, Vieira, J D, additional, Wang, L, additional, Wardlow, J, additional, and Zemcov, M, additional

Published
2018
Full Text
View/download PDF

15. The dust attenuation of star-forming galaxies at z ∼ 3 and beyond: New insights from ALMA observations

Author

Fudamoto, Y., primary, Oesch, P. A., additional, Schinnerer, E., additional, Groves, B., additional, Karim, A., additional, Magnelli, B., additional, Sargent, M. T., additional, Cassata, P., additional, Lang, P., additional, Liu, D., additional, Le Fèvre, O., additional, Leslie, S., additional, Smolčić, V., additional, and Tasca, L., additional

Published
2017
Full Text
View/download PDF

16. ALMA constraints on star-forming gas in a prototypical z = 1.5 clumpy galaxy: the dearth of CO(5−4) emission from UV-bright clumps

Author

Cibinel, A., primary, Daddi, E., additional, Bournaud, F., additional, Sargent, M. T., additional, le Floc'h, E., additional, Magdis, G. E., additional, Pannella, M., additional, Rujopakarn, W., additional, Juneau, S., additional, Zanella, A., additional, Duc, P.-A., additional, Oesch, P. A., additional, Elbaz, D., additional, Jagannathan, P., additional, Nyland, K., additional, and Wang, T., additional

Published
2017
Full Text
View/download PDF

20. HELP: xid+, the probabilistic de-blender forHerschelSPIRE maps

Author

Hurley, P. D., primary, Oliver, S., additional, Betancourt, M., additional, Clarke, C., additional, Cowley, W. I., additional, Duivenvoorden, S., additional, Farrah, D., additional, Griffin, M., additional, Lacey, C., additional, Le Floc'h, E., additional, Papadopoulos, A., additional, Sargent, M., additional, Scudder, J. M., additional, Vaccari, M., additional, Valtchanov, I., additional, and Wang, L., additional

Published
2016
Full Text
View/download PDF

21. HELP: star formation as a function of galaxy environment withHerschel

Author

Duivenvoorden, S., primary, Oliver, S., additional, Buat, V., additional, Darvish, B., additional, Efstathiou, A., additional, Farrah, D., additional, Griffin, M., additional, Hurley, P. D., additional, Ibar, E., additional, Jarvis, M., additional, Papadopoulos, A., additional, Sargent, M. T., additional, Scott, D., additional, Scudder, J. M., additional, Symeonidis, M., additional, Vaccari, M., additional, Viero, M. P., additional, and Wang, L., additional

Published
2016
Full Text
View/download PDF

22. Erratum to The herschel* pep/hermes luminosity function - i. probing the evolution of PACS selected galaxies to z ̃ 4 [MNRAS 436, (2013) 2875-2876]

Author

Gruppioni, C, Pozzi, F, Rodighiero, G, Delvecchio, I, Berta, S, Pozzetti, L, Zamorani, G, Andreani, P, Cimatti, A, Ilbert, O, Le Floc'h, E, Lutz, D, Magnelli, B, Marchetti, L, Monaco, L, Nordon, R, Oliver, S, Popesso, P, Riguccini, L, Roseboom, I, Rosario, DJ, Sargent, M, Vaccari, M, Altieri, B, Aussel, H, Bongiovanni, A, Cepa, J, Daddi, E, Doḿlnguez-Śanchez, H, Elbaz, D, F̈orster Schreiber, N, Genzel, R, Iribarrem, A, Magliocchetti, M, Maiolino, R, Poglitsch, A, Ṕerez Garćla, A, Sanchez-Portal, M, Sturm, E, Tacconi, L, Valtchanov, I, Amblard, A, Arumugam, V, Bethermin, M, Bock, J, Boselli, A, Buat, V, Burgarella, D, Castro-Rodŕlguez, N, Cava, A, Chania, P, Clements, DL, Conley, A, Cooray, A, Dowell, CD, Dwek, E, Eales, S, Franceschini, A, Glenn, J, Griffin, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Nguyen, HT, O'Halloran, B, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Ṕerez-Fournon, I, Pohlen, M, Rigopoulou, D, Rowan-Robinson, M, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vigroux, L, Wang, L, Wright, G, Xu, CK, Zemcov, M, Bardelli, S, Carollo, M, Contini, T, Le F́evre, O, Lilly, S, Mainieri, V, Renzini, A, Scodeggio, M, and Zucca, E

Published
2013

23. The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z similar or equal to 4 (vol 432, pg 23, 2013)

Author

Gruppioni, C, Pozzi, F, Rodighiero, G, Delvecchio, I, Berta, S, Pozzetti, L, Zamorani, G, Andreani, P, Cimatti, A, Ilbert, O, Le Floc'h, E, Lutz, D, Magnelli, B, Marchetti, L, Monaco, P, Nordon, R, Oliver, S, Popesso, P, Riguccini, L, Roseboom, I, Rosario, DJ, Sargent, M, Vaccari, M, Altieri, B, Aussel, H, Bongiovanni, A, Cepa, J, Daddi, E, Dominguez-Sanchez, H, Elbaz, D, Schreiber, NF, Genzel, R, Iribarrem, A, Magliocchetti, M, Maiolino, R, Poglitsch, A, Garcia, AP, Sanchez-Portal, M, Sturm, E, Tacconi, L, Valtchanov, I, Amblard, A, Arumugam, V, Bethermin, M, Bock, J, Boselli, A, Buat, V, Burgarella, D, Castro-Rodriguez, N, Cava, A, Chanial, P, Clements, DL, Conley, A, Cooray, A, Dowell, CD, Dwek, E, Eales, S, Franceschini, A, Glenn, J, Griffin, M, Hatziminaoglou, E, Ibar, E, Isaak, K, Ivison, RJ, Lagache, G, Levenson, L, Lu, N, Madden, S, Maffei, B, Mainetti, G, Nguyen, HT, O'Halloran, B, Page, MJ, Panuzzo, P, Papageorgiou, A, Pearson, CP, Perez-Fournon, I, Pohlen, M, Rigopoulou, D, Rowan-Robinson, M, Schulz, B, Scott, D, Seymour, N, Shupe, DL, Smith, AJ, Stevens, JA, Symeonidis, M, Trichas, M, Tugwell, KE, Vigroux, L, Wang, L, Wright, G, Xu, CK, Zemcov, M, Bardelli, S, Carollo, M, Contini, T, Le Fevre, O, Lilly, S, Mainieri, V, Renzini, A, Scodeggio, M, and Zucca, E

Published
2013

24. ALMA constraints on star-forming gas in a prototypical z = 1.5 clumpy galaxy: the dearth of CO(5-4) emission from UV-bright clumps.

Author

Cibinel, A., Daddi, E., Bournaud, F., Sargent, M. T., le Floc'h, E., Magdis, G. E., Pannella, M., Rujopakarn, W., Juneau, S., Zanella, A., Duc, P.-A., Oesch, P. A., Elbaz, D., Jagannathan, P., Nyland, K., and Wang, T.

Subjects
GALACTIC evolution, STELLAR populations, STELLAR density (Stellar population), STAR formation
Abstract

We present deep ALMA CO(5-4) observations of a main-sequence, clumpy galaxy at z = 1.5 in the HUDF. Thanks to the ∼0″.5 resolution of the ALMA data, we can link stellar population properties to the CO(5-4) emission on scales of a few kiloparsec. We detect strong CO(5-4) emission from the nuclear region of the galaxy, consistent with the observed LIR-L'CO(5-4) correlation and indicating ongoing nuclear star formation. The CO(5-4) gas component appears more concentrated than other star formation tracers or the dust distribution in this galaxy. We discuss possible implications of this difference in terms of star formation efficiency and mass build-up at the galaxy centre. Conversely, we do not detect any CO(5-4) emission from the UV-bright clumps. This might imply that clumps have a high star formation efficiency (although they do not display unusually high specific star formation rates) and are not entirely gas dominated, with gas fractions no larger than that of their host galaxy (∼50 per cent). Stellar feedback and disc instability torques funnelling gas towards the galaxy centre could contribute to the relatively low gas content. Alternatively, clumps could fall in a more standard star formation efficiency regime if their actual star formation rates are lower than generally assumed. We find that clump star formation rates derived with several different, plausible methods can vary by up to an order of magnitude. The lowest estimates would be compatible with a CO(5-4) non-detection even for main-sequence like values of star formation efficiency and gas content. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

25. The evolution of the star formation rate function and cosmic star formation rate density of galaxies at z ~ 1-4.

Author

Katsianis, A., Tescari, E., Blanc, G., and Sargent, M.

Subjects
STELLAR evolution, PARTICLE dynamics analysis, HYDRODYNAMICS, ACTIVE galactic nuclei, REDSHIFT
Abstract

We investigate the evolution of the galaxy star formation rate function (SFRF) and cosmic star formation rate density (CSFRD) of z ~ 1-4 galaxies, using cosmological smoothed particle hydrodynamic (SPH) simulations and a compilation of ultraviolet (UV), infrared (IR) and Ha observations. These tracers represent different populations of galaxies with the IR light being a probe of objects with high star formation rates and dust contents, while UV and Ha observations provide a census of low star formation galaxies where mild obscuration occurs. We compare the above SFRFs with the results of SPH simulations run with the code P-GADGET3(XXL). We focus on the role of feedback from active galactic nuclei (AGN) and supernovae in form of galactic winds. The AGN feedback prescription that we use decreases the simulated CSFRD at z < 3 but is not sufficient to reproduce the observed evolution at higher redshifts. We explore different wind models and find that the key factor for reproducing the evolution of the observed SFRF and CSFRD at z ~ 1-4 is the presence of a feedback prescription that is prominent at high redshifts (z = 4) and becomes less efficient with time. We show that variable galactic winds which are efficient at decreasing the SFRs of low-mass objects are quite successful in reproducing the observables. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

28. Erratum: The Herschel★ PEP/HerMES Luminosity Function – I. Probing the Evolution of PACS selected Galaxies to z ≃ 4

Author

Gruppioni, C., primary, Pozzi, F., additional, Rodighiero, G., additional, Delvecchio, I., additional, Berta, S., additional, Pozzetti, L., additional, Zamorani, G., additional, Andreani, P., additional, Cimatti, A., additional, Ilbert, O., additional, Le Floc'h, E., additional, Lutz, D., additional, Magnelli, B., additional, Marchetti, L., additional, Monaco, P., additional, Nordon, R., additional, Oliver, S., additional, Popesso, P., additional, Riguccini, L., additional, Roseboom, I., additional, Rosario, D. J., additional, Sargent, M., additional, Vaccari, M., additional, Altieri, B., additional, Aussel, H., additional, Bongiovanni, A., additional, Cepa, J., additional, Daddi, E., additional, Domínguez-Sánchez, H., additional, Elbaz, D., additional, Schreiber, N. Förster, additional, Genzel, R., additional, Iribarrem, A., additional, Magliocchetti, M., additional, Maiolino, R., additional, Poglitsch, A., additional, García, A. Pérez, additional, Sanchez-Portal, M., additional, Sturm, E., additional, Tacconi, L., additional, Valtchanov, I., additional, Amblard, A., additional, Arumugam, V., additional, Bethermin, M., additional, Bock, J., additional, Boselli, A., additional, Buat, V., additional, Burgarella, D., additional, Castro-Rodríguez, N., additional, Cava, A., additional, Chanial, P., additional, Clements, D. L., additional, Conley, A., additional, Cooray, A., additional, Dowell, C. D., additional, Dwek, E., additional, Eales, S., additional, Franceschini, A., additional, Glenn, J., additional, Griffin, M., additional, Hatziminaoglou, E., additional, Ibar, E., additional, Isaak, K., additional, Ivison, R. J., additional, Lagache, G., additional, Levenson, L., additional, Lu, N., additional, Madden, S., additional, Maffei, B., additional, Mainetti, G., additional, Nguyen, H. T., additional, O'Halloran, B., additional, Page, M. J., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Pearson, C. P., additional, Pérez-Fournon, I., additional, Pohlen, M., additional, Rigopoulou, D., additional, Rowan-Robinson, M., additional, Schulz, B., additional, Scott, D., additional, Seymour, N., additional, Shupe, D. L., additional, Smith, A. J., additional, Stevens, J. A., additional, Symeonidis, M., additional, Trichas, M., additional, Tugwell, K. E., additional, Vigroux, L., additional, Wang, L., additional, Wright, G., additional, Xu, C. K., additional, Zemcov, M., additional, Bardelli, S., additional, Carollo, M., additional, Contini, T., additional, Le Févre, O., additional, Lilly, S., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, and Zucca, E., additional

Published
2013
Full Text
View/download PDF

29. The Herschel★ PEP/HerMES luminosity function – I. Probing the evolution of PACS selected Galaxies to z ≃ 4

Author

Gruppioni, C., primary, Pozzi, F., additional, Rodighiero, G., additional, Delvecchio, I., additional, Berta, S., additional, Pozzetti, L., additional, Zamorani, G., additional, Andreani, P., additional, Cimatti, A., additional, Ilbert, O., additional, Le Floc’h, E., additional, Lutz, D., additional, Magnelli, B., additional, Marchetti, L., additional, Monaco, P., additional, Nordon, R., additional, Oliver, S., additional, Popesso, P., additional, Riguccini, L., additional, Roseboom, I., additional, Rosario, D. J., additional, Sargent, M., additional, Vaccari, M., additional, Altieri, B., additional, Aussel, H., additional, Bongiovanni, A., additional, Cepa, J., additional, Daddi, E., additional, Domínguez-Sánchez, H., additional, Elbaz, D., additional, Förster Schreiber, N., additional, Genzel, R., additional, Iribarrem, A., additional, Magliocchetti, M., additional, Maiolino, R., additional, Poglitsch, A., additional, Pérez García, A., additional, Sanchez-Portal, M., additional, Sturm, E., additional, Tacconi, L., additional, Valtchanov, I., additional, Amblard, A., additional, Arumugam, V., additional, Bethermin, M., additional, Bock, J., additional, Boselli, A., additional, Buat, V., additional, Burgarella, D., additional, Castro-Rodríguez, N., additional, Cava, A., additional, Chanial, P., additional, Clements, D. L., additional, Conley, A., additional, Cooray, A., additional, Dowell, C. D., additional, Dwek, E., additional, Eales, S., additional, Franceschini, A., additional, Glenn, J., additional, Griffin, M., additional, Hatziminaoglou, E., additional, Ibar, E., additional, Isaak, K., additional, Ivison, R. J., additional, Lagache, G., additional, Levenson, L., additional, Lu, N., additional, Madden, S., additional, Maffei, B., additional, Mainetti, G., additional, Nguyen, H. T., additional, O’Halloran, B., additional, Page, M. J., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Pearson, C. P., additional, Pérez-Fournon, I., additional, Pohlen, M., additional, Rigopoulou, D., additional, Rowan-Robinson, M., additional, Schulz, B., additional, Scott, D., additional, Seymour, N., additional, Shupe, D. L., additional, Smith, A. J., additional, Stevens, J. A., additional, Symeonidis, M., additional, Trichas, M., additional, Tugwell, K. E., additional, Vigroux, L., additional, Wang, L., additional, Wright, G., additional, Xu, C. K., additional, Zemcov, M., additional, Bardelli, S., additional, Carollo, M., additional, Contini, T., additional, Le Févre, O., additional, Lilly, S., additional, Mainieri, V., additional, Renzini, A., additional, Scodeggio, M., additional, and Zucca, E., additional

Published
2013
Full Text
View/download PDF

30. HELP: XID+, the probabilistic de-blender for Herschel SPIRE maps.

Author

Hurley, P. D., Oliver, S., Betancourt, M., Clarke, C., Cowley, W. I., Duivenvoorden, S., Farrah, D., Griffin, M., Lacey, C., Le Floc'h, E., Papadopoulos, A., Sargent, M., Scudder, J. M., Vaccari, M., Valtchanov, I., and Wang, L.

Subjects
ASTRONOMICAL photometry, SPECTRAL imaging, BAYESIAN analysis, PROBABILITY theory, METAPHYSICAL cosmology
Abstract

We have developed a new prior-based source extraction tool, XID+, to carry out photometry in the Herschel SPIRE (Spectral and Photometric Imaging Receiver) maps at the positions of known sources. XID+ is developed using a probabilistic Bayesian framework that provides a natural framework in which to include prior information, and uses the Bayesian inference tool Stan to obtain the full posterior probability distribution on flux estimates. In this paper, we discuss the details of XID+ and demonstrate the basic capabilities and performance by running it on simulated SPIRE maps resembling the COSMOS field, and comparing to the current prior-based source extraction tool DESPHOT. Not only we show that XID+ performs better on metrics such as flux accuracy and flux uncertainty accuracy, but we also illustrate how obtaining the posterior probability distribution can help overcome some of the issues inherent with maximum-likelihood-based source extraction routines. We run XID+ on the COSMOS SPIRE maps from Herschel Multi-Tiered Extragalactic Survey using a 24-µm catalogue as a positional prior, and a uniform flux prior ranging from 0.01 to 1000 mJy. We show the marginalized SPIRE colour--colour plot and marginalized contribution to the cosmic infrared background at the SPIRE wavelengths. XID+ is a core tool arising from the Herschel Extragalactic Legacy Project (HELP) and we discuss how additional work within HELP providing prior information on fluxes can and will be utilized. The software is available at https://github.com/H-E-L-P/XID_plus.We also provide the data product for COSMOS. We believe this is the first time that the full posterior probability of galaxy photometry has been provided as a data product. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

31. GOODS-Herschel: the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3

Author

Mullaney, J. R., primary, Pannella, M., additional, Daddi, E., additional, Alexander, D. M., additional, Elbaz, D., additional, Hickox, R. C., additional, Bournaud, F., additional, Altieri, B., additional, Aussel, H., additional, Coia, D., additional, Dannerbauer, H., additional, Dasyra, K., additional, Dickinson, M., additional, Hwang, H. S., additional, Kartaltepe, J., additional, Leiton, R., additional, Magdis, G., additional, Magnelli, B., additional, Popesso, P., additional, Valtchanov, I., additional, Bauer, F. E., additional, Brandt, W. N., additional, Del Moro, A., additional, Hanish, D. J., additional, Ivison, R. J., additional, Juneau, S., additional, Luo, B., additional, Lutz, D., additional, Sargent, M. T., additional, Scott, D., additional, and Xue, Y. Q., additional

Published
2011
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results