Browsing by Author "Bertoldi, F."

Now showing 1 - 10 of 10
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    ALMA spectroscopic survey in the Hubble Ultra Deep Field: Continuum number counts, resolved 1.2-mm extragalactic background, and properties of the faintest dusty star forming galaxies
    (2016) Bauer, Franz Erik; Aravena, M.; Decarli, R.; Walter, F.; Da Cunha, E.; Carilli, C.; Daddi, E.; Elbaz, D.; Ivison, R.; Riechers, D.; Smail, I.; Weiss, A.; Anguita, T.; Bell, E.; Bertoldi, F.; Bacon, R.
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    An ALMA survey of submillimetre galaxies in the COSMOS field : Physical properties derived from energy balance spectral energy distribution modelling
    (2017) Miettinen, O.; Delvecchio, I.; Smolčić, V.; Aravena, M.; Brisbin, D.; Karim, A.; Magnelli, B.; Novak, M.; Schinnerer, E.; Padilla, Nelson; Albrecht, M.; Aussel, H.; Bertoldi, F.; Capak, P.; Casey, C.; Hayward, C.; Ilbert , O.; Intema, H.; Jiang, C.; Le Fèvre, O.; McCracken, H.; Munõz Arancibia A.; Navarrete, F.; Riechers, D.|Salvato M.; Scott, K.; Sheth, K.; Tasca, L.
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    An ALMA survey of submillimetre galaxies in the COSMOS field : The extent of the radio-emitting region revealed by 3 GHz imaging with the Very Large Array
    (2017) Miettinen, O.; Novak, M.; Smolčić, V.; Delvecchio, I.; Aravena, M.; Brisbin, D.; Karim, A.; Murphy, E.; Schinnerer, E.; Padilla, Nelson; Albrecht, M.; Aussel, H.; Bertoldi, F.; Capak, P.; Casey, C.; Civano, F.; Hayward, C.; Herrera Ruiz, N.; Ilbert, O.; Jiang, C.; Laigle, C.; Le Fèvre, O.; Magnelli, B.; Marchesi, S.; McCracken, H.; Middelberg, E.; Muñoz Arancibia, A.; Navarrete, F.; Riechers, D.; Salvato, M.; Scott, K.; Sheth, K.; Tasca, L.; Bondi, M.; Zamorani, G.
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    H2O emission in high-z ultra-luminous infrared galaxies
    (2013) Omont, A.; Yang, C.; Cox, P.; Neri, R.; Beelen, A.; Bussmann, R. S.; Gavazzi, R.; van der Werf, P.; Riechers, D.; Downes, D.; Krips, M.; Dye, S.; Ivison, R.; Vieira, J. D.; Weiss, A.; Aguirre, J. E.; Baes, M.; Baker, A. J.; Bertoldi, F.; Cooray, A.; Dannerbauer, H.; De Zotti, G.; Eales, S. A.; Fu, H.; Gao, Y.; Guelin, M.; Harris, A. I.; Jarvis, M.; Lehnert, M.; Leeuw, L.; Lupu, R.; Menten, K.; Michalowski, M. J.; Negrello, M.; Serjeant, S.; Temi, P.; Auld, R.; Dariush, A.; Dunne, L.; Fritz, J.; Hopwood, R.; Hoyos, C.; Ibar, E.; Maddox, S.; Smith, M. W. L.; Valiante, E.; Bock, J.; Bradford, C. M.; Glenn, J.; Scott, K. S.
    Using the IRAM Plateau de Bure interferometer (PdBI), we report the detection of water vapor in six new lensed ultra-luminous starburst galaxies at high redshift, discovered in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). The sources are detected either in the 2(02)-1(11) or 2(11)-2(02) H2O emission lines with integrated line fluxes ranging from 1.8 to 14 Jy km s(-1). The corresponding apparent luminosities are mu L-H2O similar to 3-12 x 10(8) L-circle dot, where mu is the lensing magnification factor (3 < mu < 12). These results confirm that H2O lines are among the strongest molecular lines in high-z ultra-luminous starburst galaxies, with intensities almost comparable to those of the high-J CO lines, and similar profiles and line widths (similar to 200-900 km s(-1)). With the current sensitivity of the PdBI, the water lines can therefore easily be detected in high-z lensed galaxies (with F(500 mu m) > 100 mJy) discovered in the Herschel surveys. Correcting the luminosities for amplification, using existing lensing models, L-H2O is found to have a strong dependence on the infrared luminosity, varying as similar to L-IR(1.2). This relation, which needs to be confirmed with better statistics, may indicate a role of radiative (infrared) excitation of the H2O lines, and implies that high-z galaxies with L-IR greater than or similar to 10(13) L-circle dot tend to be very strong emitters in water vapor, that have no equivalent in the local universe.
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    HerMES: CANDIDATE HIGH-REDSHIFT GALAXIES DISCOVERED WITH HERSCHEL/SPIRE
    (2014) Dowell, C. Darren; Conley, A.; Glenn, J.; Arumugam, V.; Asboth, V.; Aussel, H.; Bertoldi, F.; Bethermin, M.; Bock, J.; Boselli, A.; Bridge, C.; Buat, V.; Burgarella, D.; Cabrera-Lavers, A.; Casey, C. M.; Chapman, S. C.; Clements, D. L.; Conversi, L.; Cooray, A.; Dannerbauer, H.; De Bernardis, F.; Ellsworth-Bowers, T. P.; Farrah, D.; Franceschini, A.; Griffin, M.; Gurwell, M. A.; Halpern, M.; Hatziminaoglou, E.; Heinis, S.; Ibar, E.; Ivison, R. J.; Laporte, N.; Marchetti, L.; Martinez-Navajas, P.; Marsden, G.; Morrison, G. E.; Nguyen, H. T.; O'Halloran, B.; Oliver, S. J.; Omont, A.; Page, M. J.; Papageorgiou, A.; Pearson, C. P.; Petitpas, G.; Perez-Fournon, I.; Pohlen, M.; Riechers, D.; Rigopoulou, D.; Roseboom, I. G.; Rowan-Robinson, M.; Sayers, J.; Schulz, B.; Scott, Douglas; Seymour, N.; Shupe, D. L.; Smith, A. J.; Streblyanska, A.; Symeonidis, M.; Vaccari, M.; Valtchanov, I.; Vieira, J. D.; Viero, M.; Wang, L.; Wardlow, J.; Xu, C. K.; Zemcov, M.
    We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 mu m flux densities to search for red sources. We apply this method to 21 deg(2) of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e. g., 850 mu m) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S-500 (mu m) >= 30 mJy), red Herschel sources is 3.3 +/- 0.8 deg(-2). This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z similar to 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction.
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    HERSCHEL-ATLAS: A BINARY HyLIRG PINPOINTING A CLUSTER OF STARBURSTING PROTOELLIPTICALS
    (2013) Ivison, R. J.; Swinbank, A. M.; Smail, Ian; Harris, A. I.; Bussmann, R. S.; Cooray, A.; Cox, P.; Fu, H.; Kovacs, A.; Krips, M.; Narayanan, D.; Negrello, M.; Neri, R.; Penarrubia, J.; Richard, J.; Riechers, D. A.; Rowlands, K.; Staguhn, J. G.; Targett, T. A.; Amber, S.; Baker, A. J.; Bourne, N.; Bertoldi, F.; Bremer, M.; Calanog, J. A.; Clements, D. L.; Dannerbauer, H.; Dariush, A.; De Zotti, G.; Dunne, L.; Eales, S. A.; Farrah, D.; Fleuren, S.; Franceschini, A.; Geach, J. E.; George, R. D.; Helly, J. C.; Hopwood, R.; Ibar, E.; Jarvis, M. J.; Kneib, J. -P.; Maddox, S.; Omont, A.; Scott, D.; Serjeant, S.; Smith, M. W. L.; Thompson, M. A.; Valiante, E.; Valtchanov, I.; Vieira, J.; van der Werf, P.
    Panchromatic observations of the best candidate hyperluminous infrared galaxies from the widest Herschel extragalactic imaging survey have led to the discovery of at least four intrinsically luminous z = 2.41 galaxies across an approximate to 100 kpc region-a cluster of starbursting protoellipticals. Via subarcsecond interferometric imaging we have measured accurate gas and star formation surface densities. The two brightest galaxies span similar to 3 kpc FWHM in submillimeter/radio continuum and CO J = 4-3, and double that in CO J = 1-0. The broad CO line is due partly to the multitude of constituent galaxies and partly to large rotational velocities in two counter-rotating gas disks-a scenario predicted to lead to the most intense starbursts, which will therefore come in pairs. The disks have M-dyn of several x 10(11) M-circle dot, and gas fractions of similar to 40%. Velocity dispersions are modest so the disks are unstable, potentially on scales commensurate with their radii: these galaxies are undergoing extreme bursts of star formation, not confined to their nuclei, at close to the Eddington limit. Their specific star formation rates place them greater than or similar to 5x above the main sequence, which supposedly comprises large gas disks like these. Their high star formation efficiencies are difficult to reconcile with a simple volumetric star formation law. N-body and dark matter simulations suggest that this system is the progenitor of a B(inary)-type approximate to 10(14.6)-M-circle dot cluster.
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    Measurements of co redshifts with Z-spec for lensed submillimeter galaxies discovered in the H-atlas survey.
    (2012) Lupu, R. E.; Kim, Sam; Scott, K. S.; Aguirre, J. E.; Aretxaga, I.; Auld, R.; Barton, E.; Beelen, A.; Bertoldi, F.; Bock, J. J.; Bonfield, D.
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    The ALMA Spectroscopic Survey in the HUDF : The Cosmic Dust and Gas Mass Densities in Galaxies up to z ∼ 3
    (2020) Magnelli, B.; Boogaard, L.; Decarli, R.; Gonzalez Lopez, J.; Novak, M.; Popping, G.; Smail, I.; Walter, F.; Aravena, M.; Bauer, Franz Erik; Assef, R. J.; Bertoldi, F.; Carilli, C.; Cortes, P. C.; da Cunha, E.; Daddi, E.; Diaz Santos, T.; Inami, H.; Ivison, R. J.; Le Fevre, O.; Oesch, P.; Riechers, D.; Rix, H. W.; Sargent, M. T.; van der Werf, P.; Wagg, J.; Weiss, A.
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    The ALMA Spectroscopic Survey in the HUDF: Constraining Cumulative CO Emission at 1 less than or similar to z less than or similar to 4 with Power Spectrum Analysis of ASPECS LP Data from 84 to 115 GHz
    (2019) Uzgil, B.; Carilli, C.; Lidz, A.; Walter, F.; Thyagarajan, N.; Decarli, R.; Aravena, M.; Bertoldi, F.; Cortes, P. C.; González López, Jorge
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    The evolution of the Baryons associated with Galaxies averaged over cosmic time and space
    (2020) Walter, F.; Carilli, C.; Neeleman, M.; Decarli, R.; Popping, G.; Somerville, R. S.; Aravena, M.; Bertoldi, F.; Boogaard, L.; Bauer, Franz Erik; Cox, P.; Cunha, E. da; Magnelli, B.; Obreschkow, D.; Riechers, D.; Rix, H. W.; Smail, I.; Weiss, A.; Assef, R. J.; Bouwens, R.; Contini, T.; Cortés, P. C.; Daddi, E.; Díaz Santos, T.; González López, Jorge; Hennawi, J.; Hodge, J. A.; Inami, H.; Ivison, R.; Oesch, P.; Sargent, M.; Werf, P. van der; Wagg, J.; Yung, L. Y. A.