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843 results on '"Le Fèvre, O"'

1. The size and pervasiveness of Ly α-UV spatial offsets in star-forming galaxies at z ∼6

Author

Lemaux, BC, Fuller, S, Bradač, M, Pentericci, L, Hoag, A, Strait, V, Treu, T, Alvarez, C, Bolan, P, Gandhi, PJ, Huang, KH, Jones, T, Mason, C, Pelliccia, D, Ribeiro, B, Ryan, RE, Schmidt, KB, Vanzella, E, Khusanova, Y, Le Fèvre, O, Guaita, L, Hathi, NP, Koekemoer, A, and Pforr, J

Subjects
gravitational lensing: strong, techniques: photometric, techniques: spectroscopic, galaxies: evolution, galaxies: high-redshift, reionization, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We study the projected spatial offset between the ultraviolet continuum and Ly α emission for 65 lensed and unlensed galaxies in the Epoch of Reionization (5 ≤ z ≤ 7), the first such study at these redshifts, in order to understand the potential for these offsets to confuse estimates of the Ly α properties of galaxies observed in slit spectroscopy. While we find that ∼40 per cent of galaxies in our sample show significant projected spatial offsets ($|\Delta {\rm {Ly}\alpha -\rm {UV}}|$), we find a relatively modest average projected offset of $|\widetilde{\Delta }{\rm {Ly}\alpha -\rm {UV}}|$ = 0.61 ± 0.08 proper kpc for the entire sample. A small fraction of our sample, ∼10 per cent, exhibit offsets in excess of 2 proper kpc, with offsets seen up to ∼4 proper kpc, sizes that are considerably larger than the effective radii of typical galaxies at these redshifts. An internal comparison and a comparison to studies at lower redshift yielded no significant evidence of evolution of $|\Delta {\rm {Ly}\alpha -\rm {UV}}|$ with redshift. In our sample, ultraviolet (UV)-bright galaxies ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.67$) showed offsets a factor of three greater than their fainter counterparts ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.10$), 0.89 ± 0.18 versus 0.27 ± 0.05 proper kpc, respectively. The presence of companion galaxies and early stage merging activity appeared to be unlikely causes of these offsets. Rather, these offsets appear consistent with a scenario in which internal anisotropic processes resulting from stellar feedback, which is stronger in UV-brighter galaxies, facilitate Ly α fluorescence and/or backscattering from nearby or outflowing gas. The reduction in the Ly α flux due to offsets was quantified. It was found that the differential loss of Ly α photons for galaxies with average offsets is not, if corrected for, a limiting factor for all but the narrowest slit widths (

Published
2021

2. First Data Release of the COSMOS Lyα Mapping and Tomography Observations: 3D Lyα Forest Tomography at 2.05 < z < 2.55

Author

Lee, KG, Krolewski, A, White, M, Schlegel, D, Nugent, PE, Hennawi, JF, Müller, T, Pan, R, Prochaska, JX, Font-Ribera, A, Suzuki, N, Glazebrook, K, Kacprzak, GG, Kartaltepe, JS, Koekemoer, AM, Le Fèvre, O, Lemaux, BC, Maier, C, Nanayakkara, T, Rich, RM, Sanders, DB, Salvato, M, Tasca, L, and Tran, KVH

Subjects
intergalactic medium, large-scale structure of universe, quasars: absorption lines, surveys, techniques: spectroscopic, astro-ph.CO, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

Faint star-forming galaxies at z ∼ 2-3 can be used as alternative background sources to probe the Lyα forest in addition to quasars, yielding high sightline densities that enable 3D tomographic reconstruction of the foreground absorption field. Here, we present the first data release from the COSMOS Lyα Mapping And Tomography Observations (CLAMATO) Survey, which was conducted with the LRIS spectrograph on the Keck I telescope. Over an observational footprint of 0.157 deg2 within the COSMOS field, we used 240 galaxies and quasars at 2.17 < z < 3.00, with a mean comoving transverse separation of , as background sources probing the foreground Lyα forest absorption at 2.05 < z < 2.55. The Lyα forest data was then used to create a Wiener-filtered tomographic reconstruction over a comoving volume of with an effective smoothing scale of . In addition to traditional figures, this map is also presented as a virtual-reality visualization and manipulable interactive figure. We see large overdensities and underdensities that visually agree with the distribution of coeval galaxies from spectroscopic redshift surveys in the same field, including overdensities associated with several recently discovered galaxy protoclusters in the volume. Quantitatively, the map signal-to-noise is over a 3 h -1Mpc top-hat kernel based on the variances estimated from the Wiener filter. This data release includes the redshift catalog, reduced spectra, extracted Lyα forest pixel data, and reconstructed tomographic map of the absorption. These can be downloaded from Zenodo (10.5281/zenodo.1292459).

Published
2018

3. MIDIS: Unveiling the Role of Strong H α Emitters During the Epoch of Reionization with JWST.

Author

Rinaldi, P., Caputi, K. I., Iani, E., Costantin, L., Gillman, S., Perez Gonzalez, P. G., Östlin, G., Colina, L., Greve, T. R., Nørgard-Nielsen, H. U., Wright, G. S., Álvarez-Márquez, J., Eckart, A., García-Marín, M., Hjorth, J., Ilbert, O., Kendrew, S., Labiano, A., Le Fèvre, O., and Pye, J.

Subjects
INTERSTELLAR medium, STAR formation, GALACTIC evolution, MEDIAN (Mathematics), STELLAR mass, GALACTIC redshift, STARBURSTS
Abstract

By using an ultradeep JWST/MIRI image at 5.6 μ m in the Hubble eXtreme Deep Field, we constrain the role of strong H α emitters (HAEs) during "cosmic reionization" at z ≃ 7–8. Our sample of HAEs is comprised of young (<35 Myr) galaxies, except for one single galaxy (≈300 Myr), with low stellar masses (≲109 M ⊙). These HAEs show a wide range of rest-frame UV continuum slopes (β), with a median value of β = −2.15 ± 0.21, which broadly correlates with stellar mass. We estimate the ionizing photon production efficiency (ξ ion,0) of these sources (assuming f esc,LyC = 0%), which yields a median value log 10 (ξ ion , 0 / (Hz erg − 1)) = 25.50 − 0.12 + 0.10 . We show that ξ ion,0 positively correlates with H α equivalent width and specific star formation rate. Instead ξ ion,0 weakly anticorrelates with stellar mass and β. Based on the β values, we predict f esc , LyC = 4 % − 2 + 3 , which results in log 10 (ξ ion / (Hz erg − 1)) = 25.55 − 0.13 + 0.11 . Considering this and related findings from the literature, we find a mild evolution of ξ ion with redshift. Additionally, our results suggest that these HAEs require only modest escape fractions (f esc,rel) of 6%–15% to reionize their surrounding intergalactic medium. By only considering the contribution of these HAEs, we estimated their total ionizing emissivity ( N ̇ ion ) as N ̇ ion = 10 50.53 ± 0.45 s − 1 Mpc − 3 . When comparing their N ̇ ion with non-HAE galaxies across the same redshift range, we find that that strong, young, and low-mass emitters may have played an important role during cosmic reionization. [ABSTRACT FROM AUTHOR]

Published
2024
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4. MIDIS: Strong (Hβ+[O iii]) and Hα Emitters at Redshift z ≃ 7–8 Unveiled with JWST NIRCam and MIRI Imaging in the Hubble eXtreme Deep Field

Author

Rinaldi, P., primary, Caputi, K. I., additional, Costantin, L., additional, Gillman, S., additional, Iani, E., additional, Pérez-González, P. G., additional, Östlin, G., additional, Colina, L., additional, Greve, T. R., additional, Noorgard-Nielsen, H. U., additional, Wright, G. S., additional, Alonso-Herrero, A., additional, Álvarez-Márquez, J., additional, Eckart, A., additional, García-Marín, M., additional, Hjorth, J., additional, Ilbert, O., additional, Kendrew, S., additional, Labiano, A., additional, Le Fèvre, O., additional, Pye, J., additional, Tikkanen, T., additional, Walter, F., additional, van der Werf, P., additional, Ward, M., additional, Annunziatella, M., additional, Azzollini, R., additional, Bik, A., additional, Boogaard, L., additional, Bosman, S. E. I., additional, Gómez, A. Crespo, additional, Jermann, I., additional, Langeroodi, D., additional, Melinder, J., additional, Meyer, R. A., additional, Moutard, T., additional, Peissker, F., additional, Topinka, M., additional, van Dishoeck, E., additional, Güdel, M., additional, Henning, Th., additional, Lagage, P.-O., additional, Ray, T., additional, Vandenbussche, B., additional, Waelkens, C., additional, Navarro-Carrera, R., additional, and Kokorev, V., additional

Published
2023
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5. MIRI/JWST observations reveal an extremely obscured starburst in the z = 6.9 system SPT0311-58

Author

Álvarez-márquez, J., Crespo Gómez, A., Colina, L., Neeleman, M., Walter, F., Labiano, A., Pérez-gonzález, P., Bik, A., Noorgaard-nielsen, H. U., Ostlin, G., Wright, G., Alonso-herrero, A., Azollini, R., Caputi, K. I., Eckart, A., Le Fèvre, O., García-marín, M., Greve, T. R., Hjorth, J., Ilbert, O., Kendrew, S., Pye, J. P., Tikkanen, T., Topinka, M., Van Der Werf, P., Ward, M., Van Dishoeck, E. F., Güdel, M., Henning, Th., Lagage, P. O., Ray, T., Waelkens, C., Álvarez-márquez, J., Crespo Gómez, A., Colina, L., Neeleman, M., Walter, F., Labiano, A., Pérez-gonzález, P., Bik, A., Noorgaard-nielsen, H. U., Ostlin, G., Wright, G., Alonso-herrero, A., Azollini, R., Caputi, K. I., Eckart, A., Le Fèvre, O., García-marín, M., Greve, T. R., Hjorth, J., Ilbert, O., Kendrew, S., Pye, J. P., Tikkanen, T., Topinka, M., Van Der Werf, P., Ward, M., Van Dishoeck, E. F., Güdel, M., Henning, Th., Lagage, P. O., Ray, T., and Waelkens, C.

Published
2023

6. MIRI/JWST observations reveal an extremely obscured starburst in the z = 6.9 system SPT0311-58

Author

Álvarez-Márquez, J., primary, Crespo Gómez, A., additional, Colina, L., additional, Neeleman, M., additional, Walter, F., additional, Labiano, A., additional, Pérez-González, P., additional, Bik, A., additional, Noorgaard-Nielsen, H. U., additional, Ostlin, G., additional, Wright, G., additional, Alonso-Herrero, A., additional, Azollini, R., additional, Caputi, K. I., additional, Eckart, A., additional, Le Fèvre, O., additional, García-Marín, M., additional, Greve, T. R., additional, Hjorth, J., additional, Ilbert, O., additional, Kendrew, S., additional, Pye, J. P., additional, Tikkanen, T., additional, Topinka, M., additional, van der Werf, P., additional, Ward, M., additional, van Dishoeck, E. F., additional, Güdel, M., additional, Henning, Th., additional, Lagage, P. O., additional, Ray, T., additional, and Waelkens, C., additional

Published
2023
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7. COSMOS2020: UV-selected galaxies at z ≥ 7.5

Author

Kauffmann, O. B., primary, Ilbert, O., additional, Weaver, J. R., additional, McCracken, H. J., additional, Milvang-Jensen, B., additional, Brammer, G., additional, Davidzon, I., additional, Le Fèvre, O., additional, Liu, D., additional, Mobasher, B., additional, Moneti, A., additional, Shuntov, M., additional, Toft, S., additional, Casey, C. M., additional, Dunlop, J. S., additional, Kartaltepe, J. S., additional, Koekemoer, A. M., additional, Sanders, D. B., additional, and Tresse, L., additional

Published
2022
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9. The VVDS: Early Results on the Large Scale Structure Distribution of Galaxies out to z~1.5

Author

Le Fèvre, O., Vettolani, G., Maccagni, D., Picat, J.P., Adami, C., Arnaboldi, M., Arnouts, S., Bardelli, S., Bolzonella, M., Bondi, M., Bottini, D., Busarello, G., Cappi, A., Ciliegi, P., Contini, T., Charlot, S., Foucaud, S., Franzetti, P., Garilli, B., Gavignaud, I., Guzzo, L., Ilbert, O., Iovino, A., Le Brun, V., Marano, B., Marinoni, C., McCracken, H.J., Mathez, G., Mazure, A., Mellier, Y., Meneux, B., Merluzzi, P., Merighi, R., Paltani, S., Pellò, R., Pollo, A., Pozzetti, L., Radovich, M., Rizzo, D., Scaramella, R., Scodeggio, M., Tresse, L., Zamorani, G., Zanichelli, A., Zucca, E., Renzini, Alvio, editor, and Bender, Ralf, editor

Published
2005
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10. Deep Redshift Surveys: The VIMOS VLT Deep Survey (Invited)

Author

Le Fevre, O., Vettolani, G., Maccagni, D., Picat, J. P., Adami, C., Arnaboldi, M., Bardelli, S., Bottini, D., Busarello, G., Cappi, A., Contini, T., Charlot, S., Garilli, B., Gavignaud, I., Guzzo, L., Ilbert, O., Iovino, A., Le Brun, V., Marinoni, C., McCracken, H. J., Mathez, G., Mazure, A., Mellier, Y., Meneux, B., Merluzi, P., Paltani, S., Pelló, R., Radovich, M., Scaramella, R., Scodeggio, M., Tresse, L., Zamorani, G., Zanichelli, A., Zucca, E., Burton, W. B., editor, Kuijpers, J. M. E., editor, van den Heuvel, E. P. J., editor, van der Laan, H., editor, Appenzeler, I., editor, Bahcall, J. N., editor, Bertola, F., editor, Cassinelli, J. P., editor, Cesarsky, C. J., editor, Engvold, O., editor, McCray, R., editor, Murdin, P. G., editor, Pacini, F., editor, Radhakrishnan, V., editor, Sato, K., editor, Shu, F. H., editor, Somov, B. V., editor, Sunyaev, R. A., editor, Tanaka, Y., editor, Tremaine, S., editor, Weiss, N. O., editor, and Plionis, Manolis, editor

Published
2004
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11. Clustering of High Redshift Galaxies in the Canada-France Deep Fields Survey and Virmos Deep Imaging Survey

Author

Foucaud, S., McCracken, H. J., Le Fèvre, O., Brodwin, M., Mellier, Y., Arnouts, S., Bertin, E., Crampton, D., Cuillandre, J.-C., Dantel-Fort, M., Gwyn, S. D. J., Lilly, S. J., Radovich, M., Burton, W. B., editor, Kuijpers, J. M. E., editor, van den Heuvel, E. P. J., editor, van der Laan, H., editor, Appenzeler, I., editor, Bahcall, J. N., editor, Bertola, F., editor, Cassinelli, J. P., editor, Cesarsky, C. J., editor, Engvold, O., editor, McCray, R., editor, Murdin, P. G., editor, Pacini, F., editor, Radhakrishnan, V., editor, Sato, K., editor, Shu, F. H., editor, Somov, B. V., editor, Sunyaev, R. A., editor, Tanaka, Y., editor, Tremaine, S., editor, Weiss, N. O., editor, and Plionis, Manolis, editor

Published
2004
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13. The VIRMOS-VLT Deep Survey

Author

Le Fèvre, O., Vettolani, G., Maccagni, D., Mancini, D., Mazure, A., Mellier, Y., Picat, J. P., Arnaboldi, M., Bardelli, S., Bertin, E., Busarello, G., Cappi, A., Charlot, S., Colombi, S., Garilli, B., Guzzo, L., Iovino, A., Brun, V. Le, Mathez, G., Merluzzi, P., McCracken, H. J., Pellò, R., Pozzetti, L., Radovich, M., Ripepi, V., Saracco, P., Scaramella, R., Scodeggio, M., Tresse, L., Zamorani, G., Zucca, E., Cristiani, Stefano, editor, Renzini, Alvio, editor, and Williams, Robert E., editor

Published
2001
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14. The VIMOS Ultra Deep Survey: The reversal of the star-formation rate − density relation at 2 < z < 5

Author

Lemaux, B. C., primary, Cucciati, O., additional, Le Fèvre, O., additional, Zamorani, G., additional, Lubin, L. M., additional, Hathi, N., additional, Ilbert, O., additional, Pelliccia, D., additional, Amorín, R., additional, Bardelli, S., additional, Cassata, P., additional, Gal, R. R., additional, Garilli, B., additional, Guaita, L., additional, Giavalisco, M., additional, Hung, D., additional, Koekemoer, A., additional, Maccagni, D., additional, Pentericci, L., additional, Ribeiro, B., additional, Schaerer, D., additional, Shah, E., additional, Shen, L., additional, Staab, P., additional, Talia, M., additional, Thomas, R., additional, Tomczak, A. R., additional, Tresse, L., additional, Vanzella, E., additional, Vergani, D., additional, and Zucca, E., additional

Published
2022
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15. The ALPINE-ALMA [C II] survey: Investigation of 10 galaxies at z ∼ 4.5 with [O II] and [C II] line emission − ISM properties and [O II]−SFR relation

Author

Vanderhoof, Brittany N., Faisst, A. L., Shen, L., Lemaux, B. C., Béthermin, M., Capak, P. L., Cassata, P., Le Fèvre, O., Schaerer, D., Silverman, J., Yan, L., Boquien, M., Gal, R., Kartaltepe, J., Lubin, L. M., Dessauges-Zavadsky, M., Fudamoto, Y., Ginolfi, M., Hathi, N. P., Jones, G. C., Koekemoer, A. M., Narayanan, D., Romano, M., Talia, M., Vergani, D., and Zamorani, G.

Abstract

We present 10 main-sequence ALPINE galaxies (log (M/M_⊙) = 9.2−11.1 and SFR = 23−190 M_⊙ yr⁻¹) at z ∼ 4.5 with optical [O II] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band imaging. This is the largest such multiwavelength sample at these redshifts, combining various measurements in the ultraviolet, optical, and far-infrared including [C II]_(158 μm) line emission and dust continuum from ALMA and H α emission from Spitzer photometry. For the first time, this unique sample allows us to analyse the relation between [O II] and total star-formation rate (SFR) and the interstellar medium (ISM) properties via [O II]/[C II] and [O II]/H α luminosity ratios at z ∼ 4.5. The [O II]−SFR relation at z ∼ 4.5 cannot be described using standard local descriptions, but is consistent with a metal-dependent relation assuming metallicities around 50 per cent solar. To explain the measured dust-corrected luminosity ratios of log(L_[OII]/L_[CII]) ∼ 0.98^(+0.21)_(−0.22) and log(L_[OII]/L_(Hα)) ∼ −0.22^(+0.13)_(−0.15) for our sample, ionization parameters log (U) < −2 and electron densities log(nₑ/[cm⁻³]) ∼ 2.5−3 are required. The former is consistent with galaxies at z ∼ 2−3, however lower than at z > 6. The latter may be slightly higher than expected given the galaxies’ specific SFR. The analysis of this pilot sample suggests that typical log (M/M_⊙) > 9 galaxies at z ∼ 4.5 to have broadly similar ISM properties as their descendants at z ∼ 2 and suggest a strong evolution of ISM properties since the epoch of reionization at z > 6.

Published
2022

18. The Canada France Redshift Survey

Author

Hammer, F., Lilly, S., Crampton, D., Le Fèvre, O., Flores, H., Schade, D., Kontizas, E., editor, Kontizas, M., editor, Morgan, D. H., editor, and Vettolani, G. P., editor

Published
1997
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19. The VLT-VIRMOS Deep Redshift Survey

Author

Le Fèvre, O., Vettolani, P., Cuby, J. G., Maccagni, D., Mancini, D., Mazure, A., Mellier, Y., Picat, J. P., Kontizas, E., editor, Kontizas, M., editor, Morgan, D. H., editor, and Vettolani, G. P., editor

Published
1997
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20. COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author

Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fèvre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolc̆ić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W.-H., Zamorani, G., Weaver, J. R., Kauffmann, O. B., Ilbert, O., McCracken, H. J., Moneti, A., Toft, S., Brammer, G., Shuntov, M., Davidzon, I., Hsieh, B. C., Laigle, C., Anastasiou, A., Jespersen, C. K., Vinther, J., Capak, P., Casey, C. M., McPartland, C. J. R., Milvang-Jensen, B., Mobasher, B., Sanders, D. B., Zalesky, L., Arnouts, S., Aussel, H., Dunlop, J. S., Faisst, A., Franx, M., Furtak, L. J., Fynbo, J. P. U., Gould, K. M. L., Greve, T. R., Gwyn, S., Kartaltepe, J. S., Kashino, D., Koekemoer, A. M., Kokorev, V., Le Fèvre, O., Lilly, S., Masters, D., Magdis, G., Mehta, V., Peng, Y., Riechers, D. A., Salvato, M., Sawicki, M., Scarlata, C., Scoville, N., Shirley, R., Silverman, J. D., Sneppen, A., Smolc̆ić, V., Steinhardt, C., Stern, D., Tanaka, M., Taniguchi, Y., Teplitz, H. I., Vaccari, M., Wang, W.-H., and Zamorani, G.

Abstract

The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i < 21 sources have subpercent photometric redshift accuracy and even the faintest sources at 25 < i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).

Published
2022

24. The ALPINE-ALMA [CII] survey: The population of [CII]-undetected galaxies and their role in the L[CII]-SFR relation

Author

Romano, M., primary, Morselli, L., additional, Cassata, P., additional, Ginolfi, M., additional, Schaerer, D., additional, Béthermin, M., additional, Capak, P., additional, Faisst, A., additional, Le Fèvre, O., additional, Silverman, J. D., additional, Yan, L., additional, Bardelli, S., additional, Boquien, M., additional, Dessauges-Zavadsky, M., additional, Fujimoto, S., additional, Hathi, N. P., additional, Jones, G. C., additional, Koekemoer, A. M., additional, Lemaux, B. C., additional, Méndez-Hernández, H., additional, Narayanan, D., additional, Talia, M., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2022
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25. The VVDS Data‐Reduction Pipeline: Introducing VIPGI, the VIMOS Interactive Pipeline and Graphical Interface

Author

Scodeggio, M., Franzetti, P., Garilli, B., Zanichelli, A., Paltani, S., Maccagni, D., Bottini, D., Le Brun, V., Contini, T., Scaramella, R., Adami, C., Bardelli, S., Zucca, E., Tresse, L., Ilbert, O., Foucaud, S., Iovino, A., Merighi, R., Zamorani, G., Gavignaud, I., Rizzo, D., McCracken, H. J., Le Fèvre, O., Picat, J. P., Vettolani, G., Arnaboldi, M., Arnouts, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Guzzo, L., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Pellò, R., Pollo, A., Pozzetti, L., and Radovich, M.

Published
2005
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26. The VIMOS Integral Field Unit: Data‐Reduction Methods and Quality Assessment

Author

Zanichelli, A., Garilli, B., Scodeggio, M., Franzetti, P., Rizzo, D., Maccagni, D., Merighi, R., Picat, J. P., Le Fèvre, O., Foucaud, S., Bottini, D., Le Brun, V., Scaramella, R., Tresse, L., Vettolani, G., Adami, C., Arnaboldi, M., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Gavignaud, I., Guzzo, L., Ilbert, O., Iovino, A., McCracken, H. J., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Paltani, S., Pellò, R., Pollo, A., Pozzetti, L., Radovich, M., Zamorani, G., and Zucca, E.

Published
2005
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27. The Very Large Telescope Visible Multi‐Object Spectrograph Mask Preparation Software

Author

Bottini, D., Garilli, B., Maccagni, D., Tresse, L., Le Brun, V., Le Fèvre, O., Picat, J. P., Scaramella, R., Scodeggio, M., Vettolani, G., Zanichelli, A., Adami, C., Arnaboldi, M., Arnouts, S., Bardelli, S., Bolzonella, M., Cappi, A., Charlot, S., Ciliegi, P., Contini, T., Foucaud, S., Franzetti, P., Guzzo, L., Ilbert, O., Iovino, A., McCracken, H. J., Marano, B., Marinoni, C., Mathez, G., Mazure, A., Meneux, B., Merighi, R., Paltani, S., Pollo, A., Pozzetti, L., Radovich, M., Zamorani, G., and Zucca, E.

Published
2005
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28. The ALPINE-ALMA [C ii] survey: Investigation of 10 galaxies at z ∼ 4.5 with [O ii] and [C ii] line emission − ISM properties and [O ii]−SFR relation

Author

Vanderhoof, Brittany N, primary, Faisst, A L, additional, Shen, L, additional, Lemaux, B C, additional, Béthermin, M, additional, Capak, P L, additional, Cassata, P, additional, Le Fèvre, O, additional, Schaerer, D, additional, Silverman, J, additional, Yan, L, additional, Boquien, M, additional, Gal, R, additional, Kartaltepe, J, additional, Lubin, L M, additional, Dessauges-Zavadsky, M, additional, Fudamoto, Y, additional, Ginolfi, M, additional, Hathi, N P, additional, Jones, G C, additional, Koekemoer, A M, additional, Narayanan, D, additional, Romano, M, additional, Talia, M, additional, Vergani, D, additional, and Zamorani, G, additional

Published
2022
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29. COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs

Author

Weaver, J. R., primary, Kauffmann, O. B., additional, Ilbert, O., additional, McCracken, H. J., additional, Moneti, A., additional, Toft, S., additional, Brammer, G., additional, Shuntov, M., additional, Davidzon, I., additional, Hsieh, B. C., additional, Laigle, C., additional, Anastasiou, A., additional, Jespersen, C. K., additional, Vinther, J., additional, Capak, P., additional, Casey, C. M., additional, McPartland, C. J. R., additional, Milvang-Jensen, B., additional, Mobasher, B., additional, Sanders, D. B., additional, Zalesky, L., additional, Arnouts, S., additional, Aussel, H., additional, Dunlop, J. S., additional, Faisst, A., additional, Franx, M., additional, Furtak, L. J., additional, Fynbo, J. P. U., additional, Gould, K. M. L., additional, Greve, T. R., additional, Gwyn, S., additional, Kartaltepe, J. S., additional, Kashino, D., additional, Koekemoer, A. M., additional, Kokorev, V., additional, Le Fèvre, O., additional, Lilly, S., additional, Masters, D., additional, Magdis, G., additional, Mehta, V., additional, Peng, Y., additional, Riechers, D. A., additional, Salvato, M., additional, Sawicki, M., additional, Scarlata, C., additional, Scoville, N., additional, Shirley, R., additional, Silverman, J. D., additional, Sneppen, A., additional, Smolc̆ić, V., additional, Steinhardt, C., additional, Stern, D., additional, Tanaka, M., additional, Taniguchi, Y., additional, Teplitz, H. I., additional, Vaccari, M., additional, Wang, W.-H., additional, and Zamorani, G., additional

Published
2022
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30. The VLT‐VIRMOS Mask Manufacturing Unit

Author

Conti, G., Mattaini, E., Chiappetti, L., Maccagni, D., Sant’Ambrogio, E., Bottini, D., Garilli, B., Le Fèvre, O., Saisse, M., Voët, C., Caputi, O., Cascone, E., Mancini, D., Mancini, G., Perrotta, F., Schipani, P., and Vettolani, G.

Published
2001
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31. The size and pervasiveness of Ly α–UV spatial offsets in star-forming galaxies at z ∼ 6

Author

Lemaux, BC, Fuller, S, Bradač, M, Pentericci, L, Hoag, A, Strait, V, Treu, T, Alvarez, C, Bolan, P, Gandhi, PJ, Huang, K-H, Jones, T, Mason, C, Pelliccia, D, Ribeiro, B, Ryan, RE, Schmidt, KB, Vanzella, E, Khusanova, Y, Le Fèvre, O, Guaita, L, Hathi, NP, Koekemoer, A, and Pforr, J

Subjects
photometric [techniques], strong [gravitational lensing], astro-ph.GA, reionization, spectroscopic [techniques], Astronomy & Astrophysics, evolution [galaxies], high-redshift [galaxies], Astronomical and Space Sciences
Abstract

We study the projected spatial offset between the ultraviolet continuum and Ly α emission for 65 lensed and unlensed galaxies in the Epoch of Reionization (5 ≤ z ≤ 7), the first such study at these redshifts, in order to understand the potential for these offsets to confuse estimates of the Ly α properties of galaxies observed in slit spectroscopy. While we find that ∼40 per cent of galaxies in our sample show significant projected spatial offsets ($|\Delta {\rm {Ly}\alpha -\rm {UV}}|$), we find a relatively modest average projected offset of $|\widetilde{\Delta }{\rm {Ly}\alpha -\rm {UV}}|$ = 0.61 ± 0.08 proper kpc for the entire sample. A small fraction of our sample, ∼10 per cent, exhibit offsets in excess of 2 proper kpc, with offsets seen up to ∼4 proper kpc, sizes that are considerably larger than the effective radii of typical galaxies at these redshifts. An internal comparison and a comparison to studies at lower redshift yielded no significant evidence of evolution of $|\Delta {\rm {Ly}\alpha -\rm {UV}}|$ with redshift. In our sample, ultraviolet (UV)-bright galaxies ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.67$) showed offsets a factor of three greater than their fainter counterparts ($\widetilde{L{\mathrm{ UV}}}/L{\ast }{\mathrm{ UV}}=0.10$), 0.89 ± 0.18 versus 0.27 ± 0.05 proper kpc, respectively. The presence of companion galaxies and early stage merging activity appeared to be unlikely causes of these offsets. Rather, these offsets appear consistent with a scenario in which internal anisotropic processes resulting from stellar feedback, which is stronger in UV-brighter galaxies, facilitate Ly α fluorescence and/or backscattering from nearby or outflowing gas. The reduction in the Ly α flux due to offsets was quantified. It was found that the differential loss of Ly α photons for galaxies with average offsets is not, if corrected for, a limiting factor for all but the narrowest slit widths (

Published
2021

32. Obscured star formation rate density and main sequence of star-forming galaxies at z > 4

Author

Khusanova, Y, Bethermin, M, Le Fèvre, O, Capak, P, Faisst, A, Schaerer, D, Silverman, J, Cassata, P, Yan, L, Ginolfi, M, Fudamoto, Y, Loiacono, F, Amorin, R, Bardelli, S, Boquien, M, Cimatti, A, Dessauges-Zavadsky, M, Gruppioni, C, Hathi, N, Jones, G, Koekemoer, A, Lagache, G, Maiolino, R, Lemaux, B, Oesch, P, Pozzi, F, Riechers, D, Romano, M, Talia, M, Toft, S, Vergani, D, Zamorani, G, Zucca, E, 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), California Institute of Technology (CALTECH), Université de Genève = University of Geneva (UNIGE), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Universidad de La Serena (USERENA), Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Universidad de Antofagasta, Space Telescope Science Institute (STSci), University of Cambridge [UK] (CAM), University of California (UC), Cornell University [New York], Università degli Studi di Padova = University of Padua (Unipd), University of Copenhagen = Københavns Universitet (UCPH), European Project: 268107,EC:FP7:ERC,ERC-2010-AdG_20100224,EARLY(2011), European Project: 788212,CONCERTO, European Project: 695671,H2020,ERC-2015-AdG,QUENCH(2016), European Project: 648179,H2020,ERC-2014-CoG,ConTExt(2015), 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), Université de Genève (UNIGE), Università degli Studi di Bologna, University of California, Universita degli Studi di Padova, and University of Copenhagen = Københavns Universitet (KU)

Subjects
high-redshift -galaxies, evolution -galaxies, [PHYS]Physics [physics], galaxies, star formation -submillimeter
Abstract

International audience; Star formation rate (SFR) measurements at z > 4 have relied mostly on the rest-frame far-ultraviolet (FUV) observations. The corrections for dust attenuation based on the IRX-β relation are highly uncertain and are still debated in the literature. Hence, rest-frame far-infrared (FIR) observations are necessary to constrain the dust-obscured component of the SFR. In this paper, we exploit the rest-frame FIR continuum observations collected by the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) to directly constrain the obscured SFR in galaxies at 4.4 < z < 5.9. We used stacks of continuum images to measure average infrared luminosities taking both detected and undetected sources into account. Based on these measurements, we measured the position of the main sequence of star-forming galaxies and the specific SFR (sSFR) at z ∼ 4.5 and z ∼ 5.5. We find that the main sequence and sSFR do not significantly evolve between z ∼ 4.5 and z ∼ 5.5, as opposed to lower redshifts. We developed a method to derive the obscured SFR density (SFRD) using the stellar masses or FUV-magnitudes as a proxy of FIR fluxes measured on the stacks and combining them with the galaxy stellar mass functions and FUV luminosity functions from the literature. We obtain consistent results independent of the chosen proxy. We find that the obscured fraction of SFRD is decreasing with increasing redshift, but even at z ∼ 5.5 it constitutes around 61% of the total SFRD.

Published
2021
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33. The ALPINE-ALMA [CII] survey

Author

Pozzi, F., primary, Calura, F., additional, Fudamoto, Y., additional, Dessauges-Zavadsky, M., additional, Gruppioni, C., additional, Talia, M., additional, Zamorani, G., additional, Bethermin, M., additional, Cimatti, A., additional, Enia, A., additional, Khusanova, Y., additional, Decarli, R., additional, Le Fèvre, O., additional, Capak, P., additional, Cassata, P., additional, Faisst, A. L., additional, Yan, L., additional, Schaerer, D., additional, Silverman, J., additional, Bardelli, S., additional, Boquien, M., additional, Narayanan, D., additional, Ginolfi, M., additional, Hathi, N. P., additional, Jones, G. C., additional, Koekemoer, A. M., additional, Lemaux, B. C., additional, Loiacono, F., additional, Maiolino, R., additional, Riechers, D. A., additional, Rodighiero, G., additional, Romano, M., additional, Vallini, L., additional, Vergani, D., additional, and Zucca, E., additional

Published
2021
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34. The ALPINE-ALMA [CII] survey

Author

Romano, M., primary, Cassata, P., additional, Morselli, L., additional, Jones, G. C., additional, Ginolfi, M., additional, Zanella, A., additional, Béthermin, M., additional, Capak, P., additional, Faisst, A., additional, Le Fèvre, O., additional, Schaerer, D., additional, Silverman, J. D., additional, Yan, L., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Dessauges-Zavadsky, M., additional, Enia, A., additional, Fujimoto, S., additional, Gruppioni, C., additional, Hathi, N. P., additional, Ibar, E., additional, Koekemoer, A. M., additional, Lemaux, B. C., additional, Rodighiero, G., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2021
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35. The ALPINE-ALMA [C ii] Survey: kinematic diversity and rotation in massive star-forming galaxies at z ~ 4.4–5.9

Author

Jones, G C, primary, Vergani, D, additional, Romano, M, additional, Ginolfi, M, additional, Fudamoto, Y, additional, Béthermin, M, additional, Fujimoto, S, additional, Lemaux, B C, additional, Morselli, L, additional, Capak, P, additional, Cassata, P, additional, Faisst, A, additional, Le Fèvre, O, additional, Schaerer, D, additional, Silverman, J D, additional, Yan, Lin, additional, Boquien, M, additional, Cimatti, A, additional, Dessauges-Zavadsky, M, additional, Ibar, E, additional, Maiolino, R, additional, Rizzo, F, additional, Talia, M, additional, and Zamorani, G, additional

Published
2021
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36. An optical observational cluster mass function at z ∼ 1 with the ORELSE survey

Author

Hung, D., Lemaux, B. C., Gal, R. R., Tomczak, A. R., Lubin, L.M., Cucciati, O., Pelliccia, D., Shen, L., Le Fèvre, O., Zamorani, G., Wu, P.-F., Kocevski, D. D., Fassnacht, C.D., and Squires, G. K.

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

We present a new mass function of galaxy clusters and groups using optical/near-infrared (NIR) wavelength spectroscopic and photometric data from the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. At z ∼ 1, cluster mass function studies are rare regardless of wavelength and have never been attempted from an optical/NIR perspective. This work serves as a proof of concept that z ∼ 1 cluster mass functions are achievable without supplemental X-ray or Sunyaev-Zel’dovich data. Measurements of the cluster mass function provide important contraints on cosmological parameters and are complementary to other probes. With ORELSE, a new cluster finding technique based on Voronoi tessellation Monte Carlo (VMC) mapping, and rigorous purity and completeness testing, we have obtained ∼240 galaxy overdensity candidates in the redshift range 0.55 < z < 1.37 at a mass range of 13.6 < log (M/M⊙) < 14.8. This mass range is comparable to existing optical cluster mass function studies for the local universe. Our candidate numbers vary based on the choice of multiple input parameters related to detection and characterization in our cluster finding algorithm, which we incorporated into the mass function analysis through a Monte Carlo scheme. We find cosmological constraints on the matter density, Ω_m, and the amplitude of fluctuations, σ₈, of Ω_m = 0.250−0.099+0.104 and σ₈ = 1.150−0.163+0.260⁠. While our Ω_m value is close to concordance, our σ₈ value is ∼2σ higher because of the inflated observed number densities compared to theoretical mass function models owing to how our survey targeted overdense regions. With Euclid and several other large, unbiased optical surveys on the horizon, VMC mapping will enable optical/NIR cluster cosmology at redshifts much higher than what has been possible before.

Published
2021

37. The VANDELS ESO public spectroscopic survey

Author

Garilli, B., Mclure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., Mcleod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Calabrò, A., Cresci, G., Fynbo, J., Hathi, N., Hibon, P., Koekemoer, A., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E., Bowler, R., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Le Fèvre, O., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L., Thomas, R., Vanzella, E., Wild, V., Williams, C., Zucca, E., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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
[PHYS]Physics [physics], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, cosmology: observations, galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: statistics, catalogs, Astrophysics::Galaxy Astrophysics
Abstract

International audience; VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high-signal-to-noise ratio, medium-resolution spectra of galaxies at redshifts between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We provide a detailed description of sample selection, observations, and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at i AB = 25. The high signal-to-noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5 Å allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-infrared photometry and physical parameters derived through fitting the spectral energy distribution. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range of 8.3 < Log( M * / M ⊙ ) < 11.7.

Published
2021
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38. The ALPINE-ALMA [CII] survey: Survey strategy, observations, and sample properties of 118 star-forming galaxies at 4 < z < 6

Author

Le Fèvre, O, Béthermin, M, Faisst, A, Jones, GC, Capak, P, Cassata, P, Silverman, JD, Schaerer, D, Yan, L, Amorin, R, Bardelli, S, Boquien, M, Cimatti, A, Dessauges-Zavadsky, M, Giavalisco, M, Hathi, NP, Fudamoto, Y, Fujimoto, S, Ginolfi, M, Gruppioni, C, Hemmati, S, Ibar, E, Koekemoer, A, Khusanova, Y, Lagache, G, Lemaux, BC, Loiacono, F, Maiolino, R, Mancini, C, Narayanan, D, Morselli, L, Méndez-Hernàndez, H, Oesch, PA, Pozzi, F, Romano, M, Riechers, D, Scoville, N, Talia, M, Tasca, LAM, Thomas, R, Toft, S, Vallini, L, Vergani, D, Walter, F, Zamorani, G, Zucca, E, Jones, Gareth [0000-0002-0267-9024], Maiolino, Roberto [0000-0002-4985-3819], and Apollo - University of Cambridge Repository

Subjects
galaxies: star formation, galaxies: formation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract

The ALMA-ALPINE [CII] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [CII]-158 μm line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 4 < z < 6. We present the survey science goals, the observational strategy, and the sample selection of the 118 galaxies observed with ALMA, with an average beam minor axis of about 0.85″, or ∼5 kpc at the median redshift of the survey. The properties of the sample are described, including spectroscopic redshifts derived from the UV-rest frame, stellar masses, and star-formation rates obtained from a spectral energy distribution (SED) fitting. The observed properties derived from the ALMA data are presented and discussed in terms of the overall detection rate in [CII] and FIR continuum, with the observed signal-to-noise distribution. The sample is representative of the SFG population in the main sequence at these redshifts. The overall detection rate in [CII] is 64% for a signal-to-noise ratio (S/N) threshold larger than 3.5 corresponding to a 95% purity (40% detection rate for S/N > 5). Based on a visual inspection of the [CII] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4 < z < 6, a key epoch in galaxy assembly, which is ideally suited for studies with future facilities, such as the James Webb Space Telescope (JWST) and the Extremely Large Telescopes (ELTs).

Published
2021
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39. Less and more IGM-transmitted galaxies from z ∼ 2.7 to z ∼ 6 from VANDELS and VUDS

Author

Thomas, R., primary, Pentericci, L., additional, Le Fèvre, O., additional, Koekemoer, A. M., additional, Castellano, M., additional, Cimatti, A., additional, Fontanot, F., additional, Gargiulo, A., additional, Garilli, B., additional, Talia, M., additional, Amorín, R., additional, Bardelli, S., additional, Cristiani, S., additional, Cresci, G., additional, Franco, M., additional, Fynbo, J. P. U., additional, Hathi, N. P., additional, Hibon, P., additional, Khusanova, Y., additional, Le Brun, V., additional, Lemaux, B. C., additional, Mannucci, F., additional, Schaerer, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2021
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40. The ALPINE-ALMA [CII] survey

Author

Khusanova, Y., primary, Bethermin, M., additional, Le Fèvre, O., additional, Capak, P., additional, Faisst, A. L., additional, Schaerer, D., additional, Silverman, J. D., additional, Cassata, P., additional, Yan, L., additional, Ginolfi, M., additional, Fudamoto, Y., additional, Loiacono, F., additional, Amorin, R., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Dessauges-Zavadsky, M., additional, Gruppioni, C., additional, Hathi, N. P., additional, Jones, G. C., additional, Koekemoer, A. M., additional, Lagache, G., additional, Maiolino, R., additional, Lemaux, B. C., additional, Oesch, P., additional, Pozzi, F., additional, Riechers, D. A., additional, Romano, M., additional, Talia, M., additional, Toft, S., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2021
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41. Gravitational magnification effects on distant 3CR galaxies

Author

Le Fevre, O., Hammer, F., Araki, H., editor, Ehlers, J., editor, Hepp, K., editor, Kippenhahn, R., editor, Ruelle, D., editor, Weidenmüller, H. A., editor, Wess, J., editor, Zittartz, J., editor, Beiglböck, W., editor, Mellier, Yannick, editor, Fort, Bernard, editor, and Soucail, Geneviève, editor

Published
1990
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42. The ALPINE-ALMA [C II] survey. Dust attenuation properties and obscured star formation at z ∼ 4.4–5.8

Author

Fudamoto, Y., Oesch, P. A., Faisst, A., Béthermin, M., Ginolfi, M., Khusanova, Y., Loiacono, F., Le Fèvre, O., Capak, P., Schaerer, D., Silverman, J. D., Cassata, P., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Fujimoto, S., Gruppioni, C., Hathi, N. P., Ibar, E., Jones, G. C., Koekemoer, A. M., Lagache, G., Lemaux, B. C., Maiolino, R., Narayanan, D., Pozzi, F., Riechers, D. A., Rodighiero, G., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., and Zucca, E.

Abstract

We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 − 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [C II] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M⋆), and infrared excess (IRX = L_(IR)/L_(UV)). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 − 5.8. The individual detections and stacks show that the IRX–β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z < 4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX–β relation as a function of redshift suggests an evolution of dust attenuation properties at z > 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX–M⋆ relations at z ≲ 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z ≳ 4 are characterised by (i) a steeper attenuation curve than at z ≲ 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M⋆/M⊙ > 10) at z ∼ 5 − 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.

Published
2020

43. The ALPINE-ALMA [C II] survey. Little to no evolution in the [C II]–SFR relation over the last 13 Gyr

Author

Schaerer, D., Ginolfi, M., Béthermin, M., Fudamoto, Y., Oesch, P. A., Le Fèvre, O., Faisst, A., Capak, P., Cassata, P., Silverman, J. D., Yan, Lin, Jones, G. C., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Giavalisco, M., Hathi, N. P., Fujimoto, S., Ibar, E., Koekemoer, A., Lagache, G., Lemaux, B. C., Loiacono, F., Maiolino, R., Narayanan, D., Morselli, L., Méndez-Hernández, H., Pozzi, F., Riechers, D., Talia, M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., and Zucca, E.

Abstract

The [C II] 158 μm line is one of the strongest IR emission lines, which has been shown to trace the star formation rate (SFR) of galaxies in the nearby Universe, and up to z ∼ 2. Whether this is also the case at higher redshift and in the early Universe remains debated. The ALPINE survey, which targeted 118 star-forming galaxies at 4.4 < z < 5.9, provides a new opportunity to examine this question with the first statistical dataset. Using the ALPINE data and earlier measurements from the literature, we examine the relation between the [C II] luminosity and the SFR over the entire redshift range from z ∼ 4 − 8. ALPINE galaxies, which are both detected in [C II] and in dust continuum, show good agreement with the local L([C II])–SFR relation. Galaxies undetected in the continuum by ALMA are found to be over-luminous in [C II] when the UV SFR is used. After accounting for dust-obscured star formation, by an amount of SFR(IR) ≈ SFR(UV) on average, which results from two different stacking methods and SED fitting, the ALPINE galaxies show an L([C II])–SFR relation comparable to the local one. When [C II] non-detections are taken into account, the slope may be marginally steeper at high-z, although this is still somewhat uncertain. When compared homogeneously, the z > 6 [C II] measurements (detections and upper limits) do not behave very differently to the z ∼ 4 − 6 data. We find a weak dependence of L([C II])/SFR on the Lyα equivalent width. Finally, we find that the ratio L([C II])/L_(IR) ∼ (1 − 3) × 10⁻³ for the ALPINE sources, comparable to that of “normal” galaxies at lower redshift. Our analysis, which includes the largest sample (∼150 galaxies) of [C II] measurements at z > 4 available so far, suggests no or little evolution of the [C II]–SFR relation over the last 13 Gyr of cosmic time.

Published
2020

45. The ALPINE-ALMA [C II] survey

Author

Dessauges-Zavadsky, M., primary, Ginolfi, M., additional, Pozzi, F., additional, Béthermin, M., additional, Le Fèvre, O., additional, Fujimoto, S., additional, Silverman, J. D., additional, Jones, G. C., additional, Vallini, L., additional, Schaerer, D., additional, Faisst, A. L., additional, Khusanova, Y., additional, Fudamoto, Y., additional, Cassata, P., additional, Loiacono, F., additional, Capak, P. L., additional, Yan, L., additional, Amorin, R., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Gruppioni, C., additional, Hathi, N. P., additional, Ibar, E., additional, Koekemoer, A. M., additional, Lemaux, B. C., additional, Narayanan, D., additional, Oesch, P. A., additional, Rodighiero, G., additional, Romano, M., additional, Talia, M., additional, Toft, S., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2020
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46. The ALPINE-ALMA [C II] survey

Author

Schaerer, D., primary, Ginolfi, M., additional, Béthermin, M., additional, Fudamoto, Y., additional, Oesch, P. A., additional, Le Fèvre, O., additional, Faisst, A., additional, Capak, P., additional, Cassata, P., additional, Silverman, J. D., additional, Yan, Lin, additional, Jones, G. C., additional, Amorin, R., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Dessauges-Zavadsky, M., additional, Giavalisco, M., additional, Hathi, N. P., additional, Fujimoto, S., additional, Ibar, E., additional, Koekemoer, A., additional, Lagache, G., additional, Lemaux, B. C., additional, Loiacono, F., additional, Maiolino, R., additional, Narayanan, D., additional, Morselli, L., additional, Méndez-Hernàndez, H., additional, Pozzi, F., additional, Riechers, D., additional, Talia, M., additional, Toft, S., additional, Vallini, L., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2020
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47. The ALPINE-ALMA [CII] survey

Author

Cassata, P., primary, Morselli, L., additional, Faisst, A., additional, Ginolfi, M., additional, Béthermin, M., additional, Capak, P., additional, Le Fèvre, O., additional, Schaerer, D., additional, Silverman, J., additional, Yan, L., additional, Lemaux, B. C., additional, Romano, M., additional, Talia, M., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Dessauges-Zavadsky, M., additional, Fudamoto, Y., additional, Fujimoto, S., additional, Giavalisco, M., additional, Hathi, N. P., additional, Ibar, E., additional, Jones, G., additional, Koekemoer, A. M., additional, Méndez-Hernandez, H., additional, Mancini, C., additional, Oesch, P. A., additional, Pozzi, F., additional, Riechers, D. A., additional, Rodighiero, G., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2020
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48. The ALPINE-ALMA [CII] survey

Author

Le Fèvre, O., primary, Béthermin, M., additional, Faisst, A., additional, Jones, G. C., additional, Capak, P., additional, Cassata, P., additional, Silverman, J. D., additional, Schaerer, D., additional, Yan, L., additional, Amorin, R., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Dessauges-Zavadsky, M., additional, Giavalisco, M., additional, Hathi, N. P., additional, Fudamoto, Y., additional, Fujimoto, S., additional, Ginolfi, M., additional, Gruppioni, C., additional, Hemmati, S., additional, Ibar, E., additional, Koekemoer, A., additional, Khusanova, Y., additional, Lagache, G., additional, Lemaux, B. C., additional, Loiacono, F., additional, Maiolino, R., additional, Mancini, C., additional, Narayanan, D., additional, Morselli, L., additional, Méndez-Hernàndez, Hugo, additional, Oesch, P. A., additional, Pozzi, F., additional, Romano, M., additional, Riechers, D., additional, Scoville, N., additional, Talia, M., additional, Tasca, L. A. M., additional, Thomas, R., additional, Toft, S., additional, Vallini, L., additional, Vergani, D., additional, Walter, F., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2020
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49. The ALPINE-ALMA [CII] survey: Data processing, catalogs, and statistical source properties

Author

Béthermin, M., primary, Fudamoto, Y., additional, Ginolfi, M., additional, Loiacono, F., additional, Khusanova, Y., additional, Capak, P. L., additional, Cassata, P., additional, Faisst, A., additional, Le Fèvre, O., additional, Schaerer, D., additional, Silverman, J. D., additional, Yan, L., additional, Amorin, R., additional, Bardelli, S., additional, Boquien, M., additional, Cimatti, A., additional, Davidzon, I., additional, Dessauges-Zavadsky, M., additional, Fujimoto, S., additional, Gruppioni, C., additional, Hathi, N. P., additional, Ibar, E., additional, Jones, G. C., additional, Koekemoer, A. M., additional, Lagache, G., additional, Lemaux, B. C., additional, Moreau, C., additional, Oesch, P. A., additional, Pozzi, F., additional, Riechers, D. A., additional, Talia, M., additional, Toft, S., additional, Vallini, L., additional, Vergani, D., additional, Zamorani, G., additional, and Zucca, E., additional

Published
2020
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50. The ALPINE-ALMA [CII] survey

Author

Ginolfi, M., primary, Jones, G. C., additional, Béthermin, M., additional, Faisst, A., additional, Lemaux, B. C., additional, Schaerer, D., additional, Fudamoto, Y., additional, Oesch, P., additional, Dessauges-Zavadsky, M., additional, Fujimoto, S., additional, Carniani, S., additional, Le Fèvre, O., additional, Cassata, P., additional, Silverman, J. D., additional, Capak, P., additional, Yan, Lin, additional, Bardelli, S., additional, Cucciati, O., additional, Gal, R., additional, Gruppioni, C., additional, Hathi, N. P., additional, Lubin, L., additional, Maiolino, R., additional, Morselli, L., additional, Pelliccia, D., additional, Talia, M., additional, Vergani, D., additional, and Zamorani, G., additional

Published
2020
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