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1. MAGIC: Muse gAlaxy Groups In Cosmos -- A survey to probe the impact of environment on galaxy evolution over the last 8 Gyr

Author

Epinat, B., Contini, T., Mercier, W., Ciesla, L., Lemaux, B. C., Johnson, S. D., Richard, J., Brinchmann, J., Boogaard, L. A., Carton, D., Michel-Dansac, L., Bacon, R., Krajnovic, D., Finley, H., Schroetter, I., Ventou, E., Abril-Melgarejo, V., Boselli, A., Bouché, N. F., Kollatschny, W., Kovac, K., Paalvast, M., Soucail, G., Urrutia, T., and Weilbacher, P. M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We introduce the MUSE gAlaxy Groups in COSMOS (MAGIC) survey, which was built to study the impact of environment on galaxy evolution over the last 8 Gyr. It consists of 17 MUSE fields targeting 14 massive structures at intermediate redshift ($0.321.5$. The spectroscopic redshift completeness is high: in the redshift range of [OII] emitters ($0.25 \le z < 1.5$), where most of the groups are found, it globally reaches a maximum of 80% down to $z_{app}^{++}=25.9$, and locally decreases from $\sim 100$% to $\sim50$% in magnitude bins from $z_{app}^{++}=23-24$ to $z_{app}^{++}=25.5$. We find that the fraction of quiescent galaxies increases with local density and with the time spent in groups. A morphological dichotomy is also found between bulge-dominated quiescent and disk-dominated star-forming galaxies. As environment gets denser, the peak of the stellar mass distribution shifts towards $M_*>10^{10}~M_\odot$, and the fraction of galaxies with $M_*<10^9~M_\odot$ decreases significantly, even for star-forming galaxies. We also highlight peculiar features such as close groups, extended nebulae, and a gravitational arc. Our results suggest that galaxies are preprocessed in groups of increasing mass before entering rich groups and clusters. We publicly release two catalogs containing the properties of galaxies and groups, respectively., Comment: 27 pages, 22 figures, accepted for publication in A&A

Published
2023
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2. Scaling relations of z~0.25-1.5 galaxies in various environments from the morpho-kinematic analysis of the MAGIC sample

Author

Mercier, W., Epinat, B., Contini, T., Abril-Melgarejo, V., Boogaard, L., Brinchmann, J., Finley, H., Krajnović, D., Michel-Dansac, L., Ventou, E., Bouché, N., Dumoulin, J., and Pineda, Juan C. B.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The evolution of galaxies is influenced by many physical processes which may vary depending on their environment. We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic Explorer (MUSE) data of galaxies at 0.25

Published
2022
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3. Deep Hubble Space Telescope Imaging on the Extended Ly$\alpha$ Emission of a QSO at $z = 2.19$ with Damped Lyman Alpha System as a Natural Coronagraph

Author

Ding, Jiani, Cai, Zheng, Prochaska, J. Xavier, Finley, H., Fan, Xiaohui, Zheng, Zheng, Fathivavsari, H., and Petitjean, P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Recent observations suggest that proximate damped Ly$\alpha$ (PDLA) systems can be used to study the host galaxies of Quasi-stellar objects (QSOs), because the PDLAs can block the bright point-spread-function (PSF) from central QSOs. Using six-orbits of narrowband imaging with $\it{HST}$/WFC3, we present the first high resolution narrowband image of the Ly$\alpha$ emission in the PDLA trough of the QSO SDSSJ115432.67-021537.9 . We detect one major component and one minor component in the narrowband imaging. Combining the $\it{HST}$/WFC3 imaging with deep Magellan/MagE spectra, we measure that the Ly$\alpha$ flux F$_{\rm{Ly\alpha}}$ = 1.56$\pm0.10 \times10^{-16}$ $\rm{erg\ s^{-1}\ cm^{-2}}$, which is among the luminous ($\approx$ 2.7 L$^{\star}_{\rm{Ly\alpha}}$) Ly$\alpha$ emitters at $\it{z} =$ 2.19. The $\rm{Ly\alpha}$-based star formation rate (SFR) is $\sim$ 7 $\textrm{M_{\sun} \ yr^{-1}}$. These observational results favor that the star formation from the host galaxy could be the main mechanism to power the Ly$\alpha$ emission. This new method sheds new light on the study of the kinematic structure and the spatial distribution of the extended Ly$\alpha$ emitting regions around the QSO host.

Published
2020
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4. Kinematics, Turbulence and Star Formation of z ~1 Strongly Lensed Galaxies seen with MUSE

Author

Patricio, V., Richard, J., Carton, D., Contini, T., Epinat, B., Brinchmann, J., Schmidt, K. B., Krajnovic, D., Bouche, N., Weilbacher, P. M., Pello, R., Caruana, J., Maseda, M., Finley, H., Bauer, F. E., Martinez, J., Mahler, G., Lagattuta, D., Clement, B., Soucail, G., and Wisotzki, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We analyse a sample of 8 highly magnified galaxies at redshift 0.6

Published
2018
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5. The MUSE Hubble Ultra Deep Field Survey: II. Spectroscopic redshifts and comparisons to color selections of high-redshift galaxies

Author

Inami, H., Bacon, R., Brinchmann, J., Richard, J., Contini, T., Conseil, S., Hamer, S., Akhlaghi, M., Bouche, N., Clement, B., Desprez, G., Drake, A. B., Hashimoto, T., Leclercq, F., Maseda, M., Michel-Dansac, L., Paalvast, M., Tresse, L., Ventou, E., Kollatschny, W., Boogaard, L. A., Finley, H., Marino, R. A., Schaye, J., and Wisotzki, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have conducted a two-layered spectroscopic survey (1'x1' ultra deep and 3'x3' deep regions) in the Hubble Ultra Deep Field (HUDF) with the Multi Unit Spectroscopic Explorer (MUSE). The combination of a large field of view, high sensitivity, and wide wavelength coverage provides an order of magnitude improvement in spectroscopically confirmed redshifts in the HUDF; i.e., 1206 secure spectroscopic redshifts for HST continuum selected objects, which corresponds to 15% of the total (7904). The redshift distribution extends well beyond z>3 and to HST/F775W magnitudes as faint as ~30 mag (AB, 1-sigma). In addition, 132 secure redshifts were obtained for sources with no HST counterparts that were discovered in the MUSE data cubes by a blind search for emission-line features. In total, we present 1338 high quality redshifts, which is a factor of eight increase compared with the previously known spectroscopic redshifts in the same field. We assessed redshifts mainly with the spectral features [OII] at z<1.5 (473 objects) and Lya at 2.9~20% up to 28-29 mag and ~27 mag, respectively. We used the determined redshifts to test continuum color selection (dropout) diagrams of high-z galaxies. The selection condition for F336W dropouts successfully captures ~80% of the targeted z~2.7 galaxies. However, for higher redshift selections (F435W, F606W, and F775W dropouts), the success rates decrease to ~20-40%. We empirically redefine the selection boundaries to make an attempt to improve them to ~60%. The revised boundaries allow bluer colors that capture Lya emitters with high Lya equivalent widths falling in the broadbands used for the color-color selection. Along with this paper, we release the redshift and line flux catalog., Comment: 26 pages, 26 figures, 4 tables, accepted for publication in A&A (MUSE UDF Series Paper II), the redshift catalogs will be available at the CDS

Published
2017
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6. Possible Signatures of a Cold-Flow Disk from MUSE using a z=1 galaxy--quasar pair towards SDSSJ1422-0001

Author

Bouché, N., Finley, H., Schroetter, I., Murphy, M. T., Richter, P., Bacon, R., Contini, T., Richard, J., Wendt, M., Kammann, S., Epinat, B., Cantalupo, S., Straka, L. A., Schaye, J., Martin, C. L., Péroux, C., Wisotzki, L., Soto, K., Lilly, S., Carollo, C. M., Brinchmann, J., and Kollatschny, W.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use a background quasar to detect the presence of circum-galactic gas around a $z=0.91$ low-mass star forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the VLT show that the host galaxy has a dust-corrected star-formation rate (SFR) of 4.7$\pm$0.2 Msun/yr, with no companion down to 0.22 Msun/yr (5 $\sigma$) within 240 kpc (30"). Using a high-resolution spectrum (UVES) of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle $\alpha$ of only $15^\circ$), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold flow disk" extending at least 12 kpc ($3\times R_{1/2}$). We estimate the mass accretion rate $\dot M_{\rm in}$ to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the HI column density of $\log N_{\rm HI} \simeq 20.4$ obtained from a {\it HST}/COS NUV spectrum. From a detailed analysis of the low-ionization lines (e.g. ZnII, CrII, TiII, MnII, SiII), the accreting material appears to be enriched to about 0.4 $Z_\odot$ (albeit with large uncertainties: $\log Z/Z_\odot=-0.4~\pm~0.4$), which is comparable to the galaxy metallicity ($12+\log \rm O/H=8.7\pm0.2$), implying a large recycling fraction from past outflows. Blue-shifted MgII and FeII absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The MgII and FeII doublet ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent FeII* emission., Comment: 17 pages, 11 figures, in press (ApJ), minor edits after the proofs. Data available at http://muse-vlt.eu/science/j1422/

Published
2016
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7. Deep MUSE observations in the HDFS. Morpho-kinematics of distant star-forming galaxies down to $10^8$M$_\odot$

Author

Contini, T., Epinat, B., Bouché, N., Brinchmann, J., Boogaard, L. A., Ventou, E., Bacon, R., Richard, J., Weilbacher, P. M., Wisotzki, L., Krajnović, D., Vielfaure, J-B., Emsellem, E., Finley, H., Inami, H., Schaye, J., Swinbank, M., Guérou, A., Martinsson, T., Michel-Dansac, L., Schroetter, I., Shirazi, M., and Soucail, G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

(Abridged) We make use of the deepest VLT/MUSE observations performed so far on the Hubble Deep Field South (HDFS) to characterize the low-mass (< $10^{10}$M$_\odot$) galaxy population at intermediate redshift. We identify a sample of 28 spatially-resolved emission-line galaxies in the deep (27h integration time) MUSE data cube, spread over a redshift interval of 0.2 < z < 1.4. The public HST images and multi-band photometry over the HDFS are used to constrain the stellar mass and star formation rate (SFR) of the galaxies and to perform a morphological analysis. We derive the resolved ionized gas properties of these galaxies from the MUSE data and model the disk (both in 2D and with GalPaK$^{\rm 3D}$) to retrieve their intrinsic gas kinematics. We build a sample of resolved emission-line galaxies of much lower stellar mass and SFR (by $\sim$1-2 orders of magnitude) than previous 3D spectroscopic surveys. Most of the spatially-resolved MUSE-HDFS galaxies have gas kinematics consistent with disk-like rotation, but about 20% have velocity dispersions larger than the rotation velocities, and 30% are part of a close pair and/or show clear signs of recent gravitational interactions. In the high-mass regime, the MUSE-HDFS galaxies follow the Tully-Fisher relation defined from previous surveys in a similar redshift range. This scaling relation extends also to lower masses/velocities but with a higher dispersion. The MUSE-HDFS galaxies follow the scaling relations defined in the local universe between the specific angular momentum and the stellar mass. However, we find that intermediate-redshift star-forming galaxies fill a continuum transition from the spiral to elliptical local scaling relations, according to the dynamical state of the gas. This indicates that some galaxies may lose their angular momentum and become dispersion-dominated prior to becoming passive., Comment: 26 pages. Published in A&A

Published
2015
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8. POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING A z ∼ 1 GALAXY–QUASAR PAIR TOWARD SDSS J1422−0001* * Based on observations made at the ESO telescopes under program 080.A-0364 (SINFONI), 079.A-0600 (UVES), and as part of MUSE commissioning (ESO program 060.A-9100). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program ID 12522.

Author

Bouché, N, Finley, H, Schroetter, I, Murphy, MT, Richter, P, Bacon, R, Contini, T, Richard, J, Wendt, M, Kamann, S, Epinat, B, Cantalupo, S, Straka, LA, Schaye, J, Martin, CL, Péroux, C, Wisotzki, L, Soto, K, Lilly, S, Carollo, CM, Brinchmann, J, and Kollatschny, W

Subjects
galaxies: evolution, galaxies: formation, intergalactic medium, quasars: individual, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We use a background quasar to detect the presence of circumgalactic gas around a z = 0.91 low-mass star-forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope show that the galaxy has a dust-corrected star formation rate (SFR) of 4.7 ± 2.0 M⊙ yr-1, with no companion down to 0.22 M⊙ yr-1 (5σ) within 240 h-1 kpc ("30"). Using a high-resolution spectrum of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle α of only 15°), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold-flow disk" extending at least 12 kpc (3 × R1/2). We estimate the mass accretion rate Ṁin to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the H I column density of log NH I/cm-2 ≃ 20.4 obtained from a Hubble Space Telescope/COS near-UV spectrum. From a detailed analysis of the lowionization lines (e.g., Zn II, Cr II, Ti II, Mn II, Si II), the accreting material appears to be enriched to about 0.4 Z⊙ (albeit with large uncertainties: log Z/Z⊙ = -0.4 ± 0.4), which is comparable to the galaxy metallicity (12 + log O/H = 8.7 ± 0.2), implying a large recycling fraction from past outflows. Blueshifted Mg II and Fe II absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The Mg II and Fe II absorption line ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent Fe II∗ emission.

Published
2016

9. POSSIBLE SIGNATURES of A COLD-FLOW DISK from MUSE USING A z ∼ 1 GALAXY-QUASAR PAIR TOWARD SDSS J1422-0001

Author

Bouché, N, Finley, H, Schroetter, I, Murphy, MT, Richter, P, Bacon, R, Contini, T, Richard, J, Wendt, M, Kamann, S, Epinat, B, Cantalupo, S, Straka, LA, Schaye, J, Martin, CL, Péroux, C, Wisotzki, L, Soto, K, Lilly, S, Carollo, CM, Brinchmann, J, and Kollatschny, W

Subjects
galaxies: evolution, galaxies: formation, intergalactic medium, quasars: individual, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

We use a background quasar to detect the presence of circumgalactic gas around a z = 0.91 low-mass star-forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope show that the galaxy has a dust-corrected star formation rate (SFR) of 4.7 ± 2.0 M⊙ yr-1, with no companion down to 0.22 M⊙ yr-1 (5σ) within 240 h-1 kpc ("30"). Using a high-resolution spectrum of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle α of only 15°), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold-flow disk" extending at least 12 kpc (3 × R1/2). We estimate the mass accretion rate Ṁin to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the H I column density of log NH I/cm-2 ≃ 20.4 obtained from a Hubble Space Telescope/COS near-UV spectrum. From a detailed analysis of the lowionization lines (e.g., Zn II, Cr II, Ti II, Mn II, Si II), the accreting material appears to be enriched to about 0.4 Z⊙ (albeit with large uncertainties: log Z/Z⊙ = -0.4 ± 0.4), which is comparable to the galaxy metallicity (12 + log O/H = 8.7 ± 0.2), implying a large recycling fraction from past outflows. Blueshifted Mg II and Fe II absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The Mg II and Fe II absorption line ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent Fe II∗ emission.

Published
2016

10. A connection between extremely strong Damped Lyman-alpha Systems and Lyman-alpha Emitting Galaxies at small impact parameters

Author

Noterdaeme, P., Petitjean, P., Paris, I., Cai, Z., Finley, H., Ge, J., Pieri, M. M., and York, D. G.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a study of ~100 high redshift (z~2-4) extremely strong damped Lyman-alpha systems (ESDLA, with N(HI)>0.5x10^22 cm^-2) detected in quasar spectra from the Baryon Oscillation Spectroscopic Survey SDSS-III DR11. We study the neutral hydrogen, metal, and dust content of this elusive population of absorbers and confirm our previous finding that the high column density end of the N(HI) frequency distribution has a relatively shallow slope with power-law index -3.6, similar to what is seen from 21-cm maps in nearby galaxies. The stacked absorption spectrum indicates a typical metallicity ~1/20th solar, similar to the mean metallicity of the overall DLA population. The relatively small velocity extent of the low-ionisation lines suggests that ESDLAs do not arise from large-scale flows of neutral gas. The high column densities involved are in turn more similar to what is seen in DLAs associated with gamma-ray burst afterglows (GRB-DLAs), which are known to occur close to star forming regions. This indicates that ESDLAs arise from lines of sight passing at very small impact parameters from the host galaxy, as observed in nearby galaxies. This is also supported by simple theoretical considerations and recent high-z hydrodynamical simulations. We strongly substantiate this picture by the first statistical detection of Lya emission with ~(0.6+/-0.2)x10^42 erg/s in the core of ESDLAs (corresponding to about 0.1 L* at z~2-3), obtained through stacking the fibre spectra (of radius 1" corresponding to ~8 kpc at z~2.5). [truncated], Comment: 20 pages, 21 figures, 2 tables. Accepted for publication in A&A

Published
2014
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11. THE ELEVENTH and TWELFTH DATA RELEASES of the SLOAN DIGITAL SKY SURVEY: FINAL DATA from SDSS-III

Author

Alam, S, Albareti, FD, Prieto, CA, Anders, F, Anderson, SF, Anderton, T, Andrews, BH, Armengaud, E, Aubourg, É, Bailey, S, Basu, S, Bautista, JE, Beaton, RL, Beers, TC, Bender, CF, Berlind, AA, Beutler, F, Bhardwaj, V, Bird, JC, Bizyaev, D, Blake, CH, Blanton, MR, Blomqvist, M, Bochanski, JJ, Bolton, AS, Bovy, J, Bradley, AS, Brandt, WN, Brauer, DE, Brinkmann, J, Brown, PJ, Brownstein, JR, Burden, A, Burtin, E, Busca, NG, Cai, Z, Capozzi, D, Rosell, AC, Carr, MA, Carrera, R, Chambers, KC, Chaplin, WJ, Chen, YC, Chiappini, C, Chojnowski, SD, Chuang, CH, Clerc, N, Comparat, J, Covey, K, Croft, RAC, Cuesta, AJ, Cunha, K, Costa, LND, Rio, ND, Davenport, JRA, Dawson, KS, Lee, ND, Delubac, T, Deshpande, R, Dhital, S, Dutra-Ferreira, L, Dwelly, T, Ealet, A, Ebelke, GL, Edmondson, EM, Eisenstein, DJ, Ellsworth, T, Elsworth, Y, Epstein, CR, Eracleous, M, Escoffier, S, Esposito, M, Evans, ML, Fan, X, Fernández-Alvar, E, Feuillet, D, Ak, NF, Finley, H, Finoguenov, A, Flaherty, K, Fleming, SW, Font-Ribera, A, Foster, J, Frinchaboy, PM, Galbraith-Frew, JG, García, RA, García-Hernández, DA, Pérez, AEG, Gaulme, P, Ge, J, Génova-Santos, R, Georgakakis, A, Ghezzi, L, Gillespie, BA, Girardi, L, Goddard, D, Gontcho, SGA, Hernández, JIG, Grebel, EK, and Green, PJ

Subjects
atlases, catalogs, surveys, astro-ph.IM, astro-ph.GA, astro-ph.SR, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrograph, and a novel optical interferometer. All of the data from SDSS-III are now made public. In particular, this paper describes Data Release 11 (DR11) including all data acquired through 2013 July, and Data Release 12 (DR12) adding data acquired through 2014 July (including all data included in previous data releases), marking the end of SDSS-III observing. Relative to our previous public release (DR10), DR12 adds one million new spectra of galaxies and quasars from the Baryon Oscillation Spectroscopic Survey (BOSS) over an additional 3000 deg2 of sky, more than triples the number of H-band spectra of stars as part of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). The APOGEE outputs now include the measured abundances of 15 different elements for each star. In total, SDSS-III added 5200 deg2 of ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 247,216 stars over 9376 deg2; 618,080 APOGEE spectra of 156,593 stars; and 197,040 MARVELS spectra of 5513 stars. Since its first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in five bands and obtained over five million astronomical spectra.

Published
2015

12. Column density distribution and cosmological mass density of neutral gas: Sloan Digital Sky Survey-III Data Release 9

Author

Noterdaeme, P., Petitjean, P., Carithers, W. C., Pâris, I., Font-Ribera, A., Bailey, S., Aubourg, E., Bizyaev, D., Ebelke, G., Finley, H., Ge, J., Malanushenko, E., Malanushenko, V., Miralda-Escudé, J., Myers, A. D., Oravetz, D., Pan, K., Pieri, M. M., Ross, N. P., Schneider, D. P., Simmons, A., and York, D. G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the first results from an ongoing survey for Damped Lyman-alpha systems (DLAs) in the spectra of z>2 quasars observed in the course of the Baryon Oscillation Spectroscopic Survey (BOSS), which is part of the Sloan Digital Sky Survey (SDSS) III. Our full (non-statistical) sample, based on Data Release 9, comprises 12,081 systems with log N(HI)>=20, out of which 6,839 have log N(HI)>=20.3. This is the largest DLA sample ever compiled, superseding that from SDSS-II by a factor of seven. Using a statistical sub-sample and estimating systematics from realistic mock data, we probe the N(HI) distribution at = 2.5. Contrary to what is generally believed, the distribution extends beyond 10^22 cm^-2 with a moderate slope of index\approx-3.5. This result matches surprisingly well the opacity-corrected distribution observed at z = 0. The cosmological mass density of neutral gas in DLAs is found to be Omega_g_DLA~10^-3, evolving only mildly over the past 12 billion years., Comment: Accepted for publication as Letter to the Editor in A&A

Published
2012
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13. Direct Confirmation of the Asymmetry of the Cas A Supernova with Light Echoes

Author

Rest, A., Foley, R. J., Sinnott, B., Welch, D. L., Badenes, C., Filippenko, A. V., Bergmann, M., Bhatti, W. A., Blondin, S., Challis, P., Damke, G., Finley, H., Huber, M. E., Kasen, D., Kirshner, R. P., Matheson, T., Mazzali, P., Minniti, D., Nakajima, R., Narayan, G., Olsen, K., Sauer, D., Smith, R. C., and Suntzeff, N. B.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We report the first detection of asymmetry in a supernova (SN) photosphere based on SN light echo (LE) spectra of Cas A from the different perspectives of dust concentrations on its LE ellipsoid. New LEs are reported based on difference images, and optical spectra of these LEs are analyzed and compared. After properly accounting for the effects of finite dust-filament extent and inclination, we find one field where the He I and H alpha features are blueshifted by an additional ~4000 km/s relative to other spectra and to the spectra of the Type IIb SN 1993J. That same direction does not show any shift relative to other Cas A LE spectra in the Ca II near-infrared triplet feature. We compare the perspectives of the Cas A LE dust concentrations with recent three-dimensional modeling of the SN remnant (SNR) and note that the location having the blueshifted He I and H alpha features is roughly in the direction of an Fe-rich outflow and in the opposite direction of the motion of the compact object at the center of the SNR. We conclude that Cas A was an intrinsically asymmetric SN. Future LE spectroscopy of this object, and of other historical SNe, will provide additional insight into the connection of explosion mechanism to SN to SNR, as well as give crucial observational evidence regarding how stars explode., Comment: 13 pages, 7 figures, accepted for publication in ApJ

Published
2010
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14. The tenth data release of the Sloan digital sky survey: First spectroscopic data from the SDSS-iii apache point observatory galactic evolution experiment

Author

Gott, JR, Mack, CE, Ahn, CP, Alexandroff, R, Allende Prieto, C, Anders, F, Anderson, SF, Anderton, T, Andrews, BH, Aubourg, E, Bailey, S, Bastien, FA, Bautista, JE, Beers, TC, Beifiori, A, Bender, CF, Berlind, AA, Beutler, F, Bhardwaj, V, Bird, JC, Bizyaev, D, Blake, CH, Blanton, MR, Blomqvist, M, Bochanski, JJ, Bolton, AS, Borde, A, Bovy, J, Bradley, AS, Brandt, WN, Brauer, D, Brinkmann, J, Brownstein, JR, Busca, NG, Carithers, W, Carlberg, JK, Carnero, AR, Carr, MA, Chiappini, C, Chojnowski, SD, Chuang, CH, Comparat, J, Crepp, JR, Cristiani, S, Croft, RAC, Cuesta, AJ, Cunha, K, Da Costa, LN, Dawson, KS, De Lee, N, Dean, JDR, Delubac, T, Deshpande, R, Dhital, S, Ealet, A, Ebelke, GL, Edmondson, EM, Eisenstein, DJ, Epstein, CR, Escoffier, S, Esposito, M, Evans, ML, Fabbian, D, Fan, X, Favole, G, Femenía Castellá, B, Fernández Alvar, E, Feuillet, D, Filiz Ak, N, Finley, H, Fleming, SW, Font-Ribera, A, Frinchaboy, PM, Galbraith-Frew, JG, García-Hernández, DA, Pérez, AEG, Ge, J, Génova-Santos, R, Gillespie, BA, Girardi, L, González Hernández, JI, Gunn, JE, Guo, H, Halverson, S, Harding, P, Harris, DW, Hasselquist, S, Hawley, SL, Hayden, M, Hearty, FR, Herrero Davó, A, Ho, S, Hogg, DW, Holtzman, JA, Honscheid, K, Huehnerhoff, J, Ivans, II, Jackson, KM, Jiang, P, and Johnson, JA

Subjects
atlases, catalogs, surveys, astro-ph.IM, astro-ph.CO, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the Tenth Public Data Release (DR10) from its current incarnation, SDSS-III. This data release includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July. The APOGEE instrument is a near-infrared R 22,500 300 fiber spectrograph covering 1.514-1.696 μm. The APOGEE survey is studying the chemical abundances and radial velocities of roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10 includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE. Derived quantities from these spectra (radial velocities, effective temperatures, surface gravities, and metallicities) are also included. DR10 also roughly doubles the number of BOSS spectra over those included in the Ninth Data Release. DR10 includes a total of 1,507,954 BOSS spectra comprising 927,844 galaxy spectra, 182,009 quasar spectra, and 159,327 stellar spectra selected over 6373.2 deg2. © 2014. The American Astronomical Society. All rights reserved..

Published
2014

15. The Sloan Digital Sky Survey quasar catalog: ninth data release⋆

Author

Pâris, I, Petitjean, P, Aubourg, É, Bailey, S, Ross, NP, Myers, AD, Strauss, MA, Anderson, SF, Arnau, E, Bautista, J, Bizyaev, D, Bolton, AS, Bovy, J, Brandt, WN, Brewington, H, Browstein, JR, Busca, N, Capellupo, D, Carithers, W, Croft, RAC, Dawson, K, Delubac, T, Ebelke, G, Eisenstein, DJ, Engelke, P, Fan, X, Ak, N Filiz, Finley, H, Font-Ribera, A, Ge, J, Gibson, RR, Hall, PB, Hamann, F, Hennawi, JF, Ho, S, Hogg, DW, Ivezić, Ž, Jiang, L, Kimball, AE, Kirkby, D, Kirkpatrick, JA, Lee, K-G, Le Goff, J-M, Lundgren, B, MacLeod, CL, Malanushenko, E, Malanushenko, V, Maraston, C, McGreer, ID, McMahon, RG, Miralda-Escudé, J, Muna, D, Noterdaeme, P, Oravetz, D, Palanque-Delabrouille, N, Pan, K, Perez-Fournon, I, Pieri, MM, Richards, GT, Rollinde, E, Sheldon, ES, Schlegel, DJ, Schneider, DP, Slosar, A, Shelden, A, Shen, Y, Simmons, A, Snedden, S, Suzuki, N, Tinker, J, Viel, M, Weaver, BA, Weinberg, DH, White, M, Wood-Vasey, WM, and Yèche, C

Subjects
catalogs, surveys, quasars: general, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We present the Data Release 10 Quasar (DR10Q) catalog from the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey III. The catalog includes all BOSS objects that were targeted as quasar candidates during the first 2.5 years of the survey and that are confirmed as quasars via visual inspection of the spectra, have luminosities Mi[z = 2] 2.15 (117 668) is ~5 times greater than the number of z > 2.15 quasars known prior to BOSS. Redshifts and FWHMs are provided for the strongest emission lines (C iv, C iii, Mg ii). The catalog identifies 16 461 broad absorption line quasars and gives their characteristics. For each object, the catalog presents five-band (u, g, r, i, z) CCD-based photometry with typical accuracy of 0.03 mag and information on the optical morphology and selection method. The catalog also contains X-ray, ultraviolet, near-infrared, and radio emission properties of the quasars, when available, from other large-area surveys. The calibrated digital spectra cover the wavelength region 3600-10 500 Å at a spectral resolution in the range 1300 < R < 2500; the spectra can be retrieved from the SDSS Catalog Archive Server. We also provide a supplemental list of an additional 2376 quasars that have been identified among the galaxy targets of the SDSS-III/BOSS. © 2014 ESO.

Published
2012

16. Scaling relations of z ∼ 0.25–1.5 galaxies in various environments from the morpho-kinematics analysis of the MAGIC sample

Author

Mercier, W., primary, Epinat, B., additional, Contini, T., additional, Abril-Melgarejo, V., additional, Boogaard, L., additional, Brinchmann, J., additional, Finley, H., additional, Krajnović, D., additional, Michel-Dansac, L., additional, Ventou, E., additional, Bouché, N., additional, Dumoulin, J., additional, and Pineda, J. C. B., additional

Published
2022
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18. MUSE GAS FLOW and WIND (MEGAFLOW). I. FIRST MUSE RESULTS on BACKGROUND QUASARS

Author

Schroetter, I, Bouche, N, Wendt, M, Contini, T, Finley, H, Pello, R, Bacon, R, Cantalupo, S, Marino, R, Richard, J, Lilly, S, Schaye, J, Soto, K, Steinmetz, M, Straka, L, Wisotzki, L, Schroetter I., Bouche N., Wendt M., Contini T., Finley H., Pello R., Bacon R., Cantalupo S., Marino R. A., Richard J., Lilly S. J., Schaye J., Soto K., Steinmetz M., Straka L. A., Wisotzki L., Schroetter, I, Bouche, N, Wendt, M, Contini, T, Finley, H, Pello, R, Bacon, R, Cantalupo, S, Marino, R, Richard, J, Lilly, S, Schaye, J, Soto, K, Steinmetz, M, Straka, L, Wisotzki, L, Schroetter I., Bouche N., Wendt M., Contini T., Finley H., Pello R., Bacon R., Cantalupo S., Marino R. A., Richard J., Lilly S. J., Schaye J., Soto K., Steinmetz M., Straka L. A., and Wisotzki L.

Abstract

The physical properties of galactic winds are one of the keys to understand galaxy formation and evolution. These properties can be constrained thanks to background quasar lines of sight (LOS) passing near star-forming galaxies (SFGs). We present the first results of the MusE GAs FLOw and Wind survey obtained from two quasar fields, which have eight Mg ii absorbers of which three have rest equivalent width greater than 0.8. With the new Multi Unit Spectroscopic Explorer (MUSE) spectrograph on the Very Large Telescope (VLT), we detect six (75%) Mg ii host galaxy candidates within a radius of 30′′ from the quasar LOS. Out of these six galaxy-quasar pairs, from geometrical argument, one is likely probing galactic outflows, where two are classified as "ambiguous," two are likely probing extended gaseous disks and one pair seems to be a merger. We focus on the wind-pair and constrain the outflow using a high-resolution quasar spectra from the Ultraviolet and Visual Echelle Spectrograph. Assuming the metal absorption to be due to ga;s flowing out of the detected galaxy through a cone along the minor axis, we find outflow velocities in the order of ≈150 (i.e., smaller than the escape velocity) with a loading factor, , of ≈0.7. We see evidence for an open conical flow, with a low-density inner core. In the future, MUSE will provide us with about 80 multiple galaxy-quasar pairs in two dozen fields.

Published
2016

19. Evidence for ram-pressure stripping in a cluster of galaxies at z = 0.7

Author

Boselli, A., primary, Epinat, B., additional, Contini, T., additional, Abril-Melgarejo, V., additional, Boogaard, L. A., additional, Pointecouteau, E., additional, Ventou, E., additional, Brinchmann, J., additional, Carton, D., additional, Finley, H., additional, Michel-Dansac, L., additional, Soucail, G., additional, and Weilbacher, P. M., additional

Published
2019
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20. Kinematics, turbulence, and star formation of z similar to 1 strongly lensed galaxies seen with MUSE

Author

Patricio, V, Richard, J., Carton, D., Contini, T., Epinat, B., Brinchmann, J., Schmidt, K. B., Krajnovic, D., Bouche, N., Weilbacher, P. M., Pello, R., Caruana, J., Maseda, M., Finley, H., Bauer, F. E., Martinez, J., Mahler, G., Lagattuta, D., Clement, B., Soucail, G., Wisotzki, L., Patricio, V, Richard, J., Carton, D., Contini, T., Epinat, B., Brinchmann, J., Schmidt, K. B., Krajnovic, D., Bouche, N., Weilbacher, P. M., Pello, R., Caruana, J., Maseda, M., Finley, H., Bauer, F. E., Martinez, J., Mahler, G., Lagattuta, D., Clement, B., Soucail, G., and Wisotzki, L.

Published
2018

22. Kinematics, turbulence, and star formation of z ∼ 1 strongly lensed galaxies seen with MUSE

Author

Patrício, V, primary, Richard, J, additional, Carton, D, additional, Contini, T, additional, Epinat, B, additional, Brinchmann, J, additional, Schmidt, K B, additional, Krajnović, D, additional, Bouché, N, additional, Weilbacher, P M, additional, Pelló, R, additional, Caruana, J, additional, Maseda, M, additional, Finley, H, additional, Bauer, F E, additional, Martinez, J, additional, Mahler, G, additional, Lagattuta, D, additional, Clément, B, additional, Soucail, G, additional, and Wisotzki, L, additional

Published
2018
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23. Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

Author

Epinat, B., primary, Contini, T., additional, Finley, H., additional, Boogaard, L. A., additional, Guérou, A., additional, Brinchmann, J., additional, Carton, D., additional, Michel-Dansac, L., additional, Bacon, R., additional, Cantalupo, S., additional, Carollo, M., additional, Hamer, S., additional, Kollatschny, W., additional, Krajnović, D., additional, Marino, R. A., additional, Richard, J., additional, Soucail, G., additional, Weilbacher, P. M., additional, and Wisotzki, L., additional

Published
2018
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24. POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING A z similar to 1 GALAXY-QUASAR PAIR TOWARD SDSS J1422-0001

Author

Bouche, N., Finley, H., Schroetter, I., Murphy, M. T., Richter, P., Bacon, R., Contini, T., Richard, J., Wendt, M., Kamann, S., Epinat, B., Cantalupo, S., Straka, L. A., Schaye, J., Martin, C. L., Peroux, C., Wisotzki, L., Soto, K., Lilly, S., Carollo, C. M., Brinchmann, J., Kollatschny, W., 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), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
formation [galaxies], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Institut für Physik und Astronomie, intergalactic medium, Astrophysics::Cosmology and Extragalactic Astrophysics, individual (SDSS J142253.31-000149) [quasars], evolution [galaxies], Astrophysics::Galaxy Astrophysics
Abstract

International audience; We use a background quasar to detect the presence of circumgalactic gas around a z = 0.91 low-mass star-forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope show that the galaxy has a dust-corrected star formation rate (SFR) of 4.7 +/- 2.0. M-circle dot yr(-1), with no companion down to 0.22 M-circle dot yr(-1) (5 sigma) within 240 h(-1) kpc (”30”). Using a high-resolution spectrum of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle alpha of only 15 degrees), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a “cold-flow disk” extending at least 12 kpc (3 x R-1/2). We estimate the mass accretion rate M-in to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the H (I) column density of log N-H (I)/cm(-2) similar or equal to 20.4 obtained from a Hubble Space Telescope/COS near-UV spectrum. From a detailed analysis of the low-ionization lines (e.g., Zn II, Cr II, Ti II, MnII, Si II), the accreting material appears to be enriched to about 0.4 Z(circle dot) (albeit with large uncertainties: log Z/Z(circle dot) = -0.4 +/- 0.4), which is comparable to the galaxy metallicity (12 + log O/H = 8.7 +/- 0.2), implying a large recycling fraction from past outflows. Blueshifted Mg II and Fe II absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The Mg II and Fe II absorption line ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent Fe II* emission.

Published
2016

25. The MUSE Hubble Ultra Deep Field Survey

Author

Inami, H., primary, Bacon, R., additional, Brinchmann, J., additional, Richard, J., additional, Contini, T., additional, Conseil, S., additional, Hamer, S., additional, Akhlaghi, M., additional, Bouché, N., additional, Clément, B., additional, Desprez, G., additional, Drake, A. B., additional, Hashimoto, T., additional, Leclercq, F., additional, Maseda, M., additional, Michel-Dansac, L., additional, Paalvast, M., additional, Tresse, L., additional, Ventou, E., additional, Kollatschny, W., additional, Boogaard, L. A., additional, Finley, H., additional, Marino, R. A., additional, Schaye, J., additional, and Wisotzki, L., additional

Published
2017
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26. MUSE GAS FLOW AND WIND (MEGAFLOW). I. FIRST MUSE RESULTS ON BACKGROUND QUASARS

Author

Schroetter, I., primary, Bouché, N., additional, Wendt, M., additional, Contini, T., additional, Finley, H., additional, Pelló, R., additional, Bacon, R., additional, Cantalupo, S., additional, Marino, R. A., additional, Richard, J., additional, Lilly, S. J., additional, Schaye, J., additional, Soto, K., additional, Steinmetz, M., additional, Straka, L. A., additional, and Wisotzki, L., additional

Published
2016
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28. Deep MUSE observations in the HDFS

Author

Contini, T., primary, Epinat, B., additional, Bouché, N., additional, Brinchmann, J., additional, Boogaard, L. A., additional, Ventou, E., additional, Bacon, R., additional, Richard, J., additional, Weilbacher, P. M., additional, Wisotzki, L., additional, Krajnović, D., additional, Vielfaure, J-B., additional, Emsellem, E., additional, Finley, H., additional, Inami, H., additional, Schaye, J., additional, Swinbank, M., additional, Guérou, A., additional, Martinsson, T., additional, Michel-Dansac, L., additional, Schroetter, I., additional, Shirazi, M., additional, and Soucail, G., additional

Published
2016
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29. POSSIBLE SIGNATURES OF A COLD-FLOW DISK FROM MUSE USING Az∼ 1 GALAXY–QUASAR PAIR TOWARD SDSS J1422−0001

Author

Bouché, N., primary, Finley, H., additional, Schroetter, I., additional, Murphy, M. T., additional, Richter, P., additional, Bacon, R., additional, Contini, T., additional, Richard, J., additional, Wendt, M., additional, Kamann, S., additional, Epinat, B., additional, Cantalupo, S., additional, Straka, L. A., additional, Schaye, J., additional, Martin, C. L., additional, Péroux, C., additional, Wisotzki, L., additional, Soto, K., additional, Lilly, S., additional, Carollo, C. M., additional, Brinchmann, J., additional, and Kollatschny, W., additional

Published
2016
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31. Kinematics, turbulence, and star formation of z ~ 1 strongly lensed galaxies seen with MUSE.

Author

Patrício, V., Richard, J., Carton, D., Contini, T., Epinat, B., Brinchmann, J., Schmidt, K. B., Krajnović, D., Bouché, N., Weilbacher, P. M., Pelló, R., Caruana, J., Maseda, M., Finley, H., Bauer, F. E., Martinez, J., Mahler, G., Lagattuta, D., Clément, B., and Soucail, G.

Subjects
STAR formation, KINEMATICS, TURBULENCE, GALAXIES, GINI coefficient, ASTRONOMICAL photometry, ATTENUATION (Physics)
Abstract

We analyse a sample of eight highly magnified galaxies at redshift 0.6 < z < 1.5 observed with MUSE, exploring the resolved properties of these galaxies at sub-kiloparsec scales. Combining multiband HST photometry and MUSE spectra, we derive the stellar mass, global star formation rates (SFRs), extinction and metallicity from multiple nebular lines, concluding that our sample is representative of z ~ 1 star-forming galaxies. We derive the 2D kinematics of these galaxies from the [OII ] emission and model it with a new method that accounts for lensing effects and fits multiple images simultaneously. We use these models to calculate the 2D beam-smearing correction and derive intrinsic velocity dispersion maps. We find them to be fairly homogeneous, with relatively constant velocity dispersions between 15 and 80 km s-1 and Gini coefficient of ≲0.3. We do not find any evidence for higher (or lower) velocity dispersions at the positions of bright star-forming clumps. We derive resolved maps of dust attenuation and attenuation-corrected SFRs from emission lines for two objects in the sample. We use this information to study the relation between resolved SFR and velocity dispersion. We find that these quantities are not correlated, and the high-velocity dispersions found for relatively low star-forming densities seems to indicate that, at sub-kiloparsec scales, turbulence in high-z discs is mainly dominated by gravitational instability rather than stellar feedback. [ABSTRACT FROM AUTHOR]

Published
2018
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34. DIRECT CONFIRMATION OF THE ASYMMETRY OF THE CAS A SUPERNOVA WITH LIGHT ECHOES

Author

Rest, A., Foley, R. J., Sinnott, B., Welch, D. L., Badenes, C., Filippenko, A. V., Bergmann, M., Bhatti, W. A., Blondin, S., Challis, P., Damke, G., Finley, H., Huber, M. E., Kasen, D., Kirshner, R. P., Matheson, T., Mazzali, P., Minniti, D., Nakajima, R., Narayan, G., Olsen, K., Sauer, Daniel, Smith, R. C., Suntzeff, N. B., Rest, A., Foley, R. J., Sinnott, B., Welch, D. L., Badenes, C., Filippenko, A. V., Bergmann, M., Bhatti, W. A., Blondin, S., Challis, P., Damke, G., Finley, H., Huber, M. E., Kasen, D., Kirshner, R. P., Matheson, T., Mazzali, P., Minniti, D., Nakajima, R., Narayan, G., Olsen, K., Sauer, Daniel, Smith, R. C., and Suntzeff, N. B.

Abstract

We report the first detection of asymmetry in a supernova (SN) photosphere based on SN light echo (LE) spectra of Cas A from the different perspectives of dust concentrations on its LE ellipsoid. New LEs are reported based on difference images, and optical spectra of these LEs are analyzed and compared. After properly accounting for the effects of finite dust-filament extent and inclination, we find one field where the He I lambda 5876 and Ha features are blueshifted by an additional similar to 4000 km s(-1) relative to other spectra and to the spectra of the Type IIb SN 1993J. That same direction does not show any shift relative to other Cas A LE spectra in the Ca II near-infrared triplet feature. We compare the perspectives of the Cas A LE dust concentrations with recent three-dimensional modeling of the SN remnant (SNR) and note that the location having the blueshifted He I and Ha features is roughly in the direction of an Fe-rich outflow and in the opposite direction of the motion of the compact object at the center of the SNR. We conclude that Cas A was an intrinsically asymmetric SN. Future LE spectroscopy of this object, and of other historical SNe, will provide additional insight into the connection of the explosion mechanism to SN then to SNR, as well as give crucial observational evidence regarding how stars explode., authorCount :24

Published
2011
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35. The Sloan Digital Sky Survey quasar catalog: ninth data release

Author

Pâris, I., primary, Petitjean, P., additional, Aubourg, É., additional, Bailey, S., additional, Ross, N. P., additional, Myers, A. D., additional, Strauss, M. A., additional, Anderson, S. F., additional, Arnau, E., additional, Bautista, J., additional, Bizyaev, D., additional, Bolton, A. S., additional, Bovy, J., additional, Brandt, W. N., additional, Brewington, H., additional, Browstein, J. R., additional, Busca, N., additional, Capellupo, D., additional, Carithers, W., additional, Croft, R. A. C., additional, Dawson, K., additional, Delubac, T., additional, Ebelke, G., additional, Eisenstein, D. J., additional, Engelke, P., additional, Fan, X., additional, Filiz Ak, N., additional, Finley, H., additional, Font-Ribera, A., additional, Ge, J., additional, Gibson, R. R., additional, Hall, P. B., additional, Hamann, F., additional, Hennawi, J. F., additional, Ho, S., additional, Hogg, D. W., additional, Ivezić, Ž., additional, Jiang, L., additional, Kimball, A. E., additional, Kirkby, D., additional, Kirkpatrick, J. A., additional, Lee, K.-G., additional, Le Goff, J.-M., additional, Lundgren, B., additional, MacLeod, C. L., additional, Malanushenko, E., additional, Malanushenko, V., additional, Maraston, C., additional, McGreer, I. D., additional, McMahon, R. G., additional, Miralda-Escudé, J., additional, Muna, D., additional, Noterdaeme, P., additional, Oravetz, D., additional, Palanque-Delabrouille, N., additional, Pan, K., additional, Perez-Fournon, I., additional, Pieri, M. M., additional, Richards, G. T., additional, Rollinde, E., additional, Sheldon, E. S., additional, Schlegel, D. J., additional, Schneider, D. P., additional, Slosar, A., additional, Shelden, A., additional, Shen, Y., additional, Simmons, A., additional, Snedden, S., additional, Suzuki, N., additional, Tinker, J., additional, Viel, M., additional, Weaver, B. A., additional, Weinberg, D. H., additional, White, M., additional, Wood-Vasey, W. M., additional, and Yèche, C., additional

Published
2012
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36. Column density distribution and cosmological mass density of neutral gas: Sloan Digital Sky Survey-III Data Release 9

Author

Noterdaeme, P., primary, Petitjean, P., additional, Carithers, W. C., additional, Pâris, I., additional, Font-Ribera, A., additional, Bailey, S., additional, Aubourg, E., additional, Bizyaev, D., additional, Ebelke, G., additional, Finley, H., additional, Ge, J., additional, Malanushenko, E., additional, Malanushenko, V., additional, Miralda-Escudé, J., additional, Myers, A. D., additional, Oravetz, D., additional, Pan, K., additional, Pieri, M. M., additional, Ross, N. P., additional, Schneider, D. P., additional, Simmons, A., additional, and York, D. G., additional

Published
2012
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37. DIRECT CONFIRMATION OF THE ASYMMETRY OF THE CAS A SUPERNOVA WITH LIGHT ECHOES

Author

Rest, A., primary, Foley, R. J., additional, Sinnott, B., additional, Welch, D. L., additional, Badenes, C., additional, Filippenko, A. V., additional, Bergmann, M., additional, Bhatti, W. A., additional, Blondin, S., additional, Challis, P., additional, Damke, G., additional, Finley, H., additional, Huber, M. E., additional, Kasen, D., additional, Kirshner, R. P., additional, Matheson, T., additional, Mazzali, P., additional, Minniti, D., additional, Nakajima, R., additional, Narayan, G., additional, Olsen, K., additional, Sauer, D., additional, Smith, R. C., additional, and Suntzeff, N. B., additional

Published
2011
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38. A connection between extremely strong damped Lyman-α systems and Lyman-α emitting galaxies at small impact parameters.

Author

Noterdaeme, P., P. Petitjean, Pâris, I., Cai, Z., Finley, H., Ge, J., Pieri, M. M., and York, D. G.

Subjects
GALACTIC redshift, QUASARS, ABSORPTION spectra, STAR formation
Abstract

We present a study of ~100 high redshift (z ~ 2−4) extremely strong damped Lyman-α systems (ESDLA, with N(H i) ≥ 0.5 × 1022cm-2) detected in quasar spectra from the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey (SDSS-III) Data Release 11. We study the neutral hydrogen, metal, and dust content of this elusive population of absorbers and confirm our previous finding that the high column density end of the N(H i) frequency distribution has a relatively shallow slope with power-law index −3.6, similar to what is seen from 21-cm maps in nearby galaxies. The stacked absorption spectrum indicates a typical metallicity ~1/20th solar, similar to the mean metallicity of the overall DLA population. The relatively small velocity extent of the low-ionisation lines suggests that ESDLAs do not arise from large-scale flows of neutral gas. The high column densities involved are in turn more similar to what is seen in DLAs associated with gamma-ray burst afterglows (GRB-DLAs), which are known to occur close to star-forming regions. This indicates that ESDLAs arise from a line of sight passing at very small impact parameters from the host galaxy, as observed in nearby galaxies. This is also supported by simple theoretical considerations and recent high-z hydrodynamical simulations. We strongly substantiate this picture by the first statistical detection of Ly α emission with ⟨LESDLA(Ly α)⟩ ≃ (0.6 ± 0.2) × 1042 erg s-1 in the core of ESDLAs (corresponding to about 0.1 L⋆ at z ~ 2−3), obtained through stacking the fibre spectra (of radius 1 ″ corresponding to ~8 kpc at z ~ 2.5). Statistical errors on the Ly α luminosity are of the order of 0.1 × 1042 erg s-1 but we caution that the measured Ly α luminosity may be overestimated by ~35% due to sky light residuals and/or FUV emission from the quasar host and that we have neglected flux-calibration uncertainties. We estimate a more conservative uncertainty of 0.2 × 1042 erg s-1. The properties of the Ly α line (luminosity distribution, velocity width and velocity offset compared to systemic redshift) are very similar to that of the population of Lyman-α emitting galaxies (LAEs) with LLAE(Ly α) ≥ 1041erg s-1 detected in long-slit spectroscopy or narrow-band imaging surveys. By matching the incidence of ESDLAs with that of the LAEs population, we estimate the high column density gas radius to be about rgas = 2.5 kpc, i.e., significantly smaller than the radius corresponding to the BOSS fibre aperture, making fibre losses likely negligible. Finally, the average measured Ly α luminosity indicates a star-formation rate consistent with the Schmidt-Kennicutt law, SFR (M⊙ yr-1) ≈ 0.6 /fesc, where fesc < 1 is the Ly α escape fraction. Assuming the typical escape fraction of LAEs, fesc ~ 0.3, the Schmidt-Kennicutt law implies a galaxy radius of about rgal ≈ 2.5 kpc. Finally, we note that possible overestimation of the Ly α emission would result in both smaller rgas and rgal. Our results support a close association between LAEs and strong DLA host galaxies. [ABSTRACT FROM AUTHOR]

Published
2014
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42. Galactic Winds with MUSE: A Direct Detection of FeII* Emission from a z = 1.29 Galaxy

Author

Finley H. et al A. Verhamme

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Emission signatures from galactic winds provide an opportunity to directly map the outflowing gas but this is traditionally challenging because of the low surface brightness. Using deep observations (27 hours) of the Hubble Deep Field South from the Multi Unit Spectroscopic Explorer (MUSE) instrument we identify signatures of an outflow in both emission and absorption from a spatially resolved galaxy at z = 1.29 with a stellar mass M = 8 x 10^9 Msun star formation rate SFR = 77 Msun/yr and star formation rate surface brightness 1.6 Msun/kpc^2 within the [OII] half light radius R_1/2[OII] = 2.76 + 0.17 kpc. From a component of the strong resonant MgII and FeII absorptions at 350 km/s we infer a mass outflow rate that is comparable to the star formation rate. We detect non resonant FeII emission at lambda 2626 2612 2396 and 2365 at 1.2 2.4 1.5 2.7 x 10^ 18 egs s 1 cm 2 respectively. These flux ratios are consistent with the expectations for optically thick gas. By combining the four non resonant FeII emission lines we spatially map the FeII emission from an individual galaxy for the first time. The FeII emission has an elliptical morphology that is roughly aligned with the galaxy minor kinematic axis and its integrated half light radius R_1/2FeII = 4.1 + 0.4 kpc is 50 larger than the stellar continuum (R_1/2 = 2.34 + 0.17 kpc) or the [OII] nebular line. Moreover the FeII emission shows a blue wing extending up to 400 km/s which is more pronounced along the galaxy minor kinematic axis and reveals a C shaped pattern in a p v diagram along that axis. These features are consistent with a bi conical outflow.

43. "Temporary" is thought provoking.

Author

PERRY JR., FINLEY H.

Subjects
INFRASTRUCTURE (Economics), ARCHITECTURAL history
Abstract

A letter to the editor is presented in response to the article "Temporary" in the previous issue of the periodical related to description of infrastructure development of Boston, Massachusetts along with architectural history of Parthenon in Athens, Greece.

Published
2016

45. Dark Galaxy Candidates at Redshift ∼3.5 Detected with MUSE

Author

C. Diener, Roland Bacon, Lorrie A. Straka, Joseph Caruana, Jarle Brinchmann, Raffaella Anna Marino, Thierry Contini, Sofia G. Gallego, Lutz Wisotzki, H. Finley, Elena Borisova, Simon J. Lilly, Joop Schaye, Martin Wendt, Floriane Leclercq, Johan Richard, Simon Conseil, Hanae Inami, Gabriele Pezzulli, Sowgat Muzahid, Sebastiano Cantalupo, C. Marcella Carollo, Anna Marino, R, Cantalupo, S, Lilly, S, Gallego, S, Straka, L, Borisova, E, Pezzulli, G, Bacon, R, Brinchmann, J, Carollo, C, Caruana, J, Conseil, S, Contini, T, Diener, C, Finley, H, Inami, H, Leclercq, F, Muzahid, S, Richard, J, Schaye, J, Wendt, M, Wisotzki, L, Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010305 fluids & plasmas, Red shift -- Observations, galaxies: high-redshift, quasars: general, 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Cosmology -- Observations, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Galaxies -- Observations, Galaxies -- Formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, Astronomy and Astrophysics, Quasar, Galaxies, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Cosmology, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxies -- Evolution, galaxies: star formation, Dark galaxy, intergalactic medium, Equivalent width, quasars: emission line
Abstract

Recent theoretical models suggest that the early phase of galaxy formation could involve an epoch when galaxies are gas-rich but inefficient at forming stars: a "dark galaxy" phase. Here, we report the results of our MUSE (Multi Unit Spectroscopic Explorer) survey for dark galaxies fluorescently illuminated by quasars at $z>3$. Compared to previous studies which are based on deep narrow-band (NB) imaging, our integral field survey provides a nearly uniform sensitivity coverage over a large volume in redshift space around the quasars as well as full spectral information at each location. Thanks to these unique features, we are able to build control samples at large redshift distances from the quasars using the same data taken under the same conditions. By comparing the rest-frame equivalent width (EW$_{0}$) distributions of the Ly$\alpha$ sources detected in proximity to the quasars and in control samples, we detect a clear correlation between the locations of high EW$_{0}$ objects and the quasars. This correlation is not seen in other properties such as Ly$\alpha$ luminosities or volume overdensities, suggesting the possible fluorescent nature of at least some of these objects. Among these, we find 6 sources without continuum counterparts and EW$_{0}$ limits larger than $240\,\mathrm{\AA}$ that are the best candidates for dark galaxies in our survey at $z>3.5$. The volume densities and properties, including inferred gas masses and star formation efficiencies, of these dark galaxy candidates are similar to previously detected candidates at $z\approx2.4$ in NB surveys. Moreover, if the most distant of these are fluorescently illuminated by the quasar, our results also provide a lower limit of $t=60$ Myr on the quasar lifetime., Comment: 28 pages, 13 figures, 5 tables, submitted to ApJ

Published
2018

46. Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

Author

David Carton, Leindert Boogaard, Marcella Carollo, Sebastiano Cantalupo, Genevieve Soucail, Stephen Hamer, Peter M. Weilbacher, Thierry Contini, Léo Michel-Dansac, Hayley Finley, R. A. Marino, Johan Richard, Davor Krajnović, Roland Bacon, Benoît Epinat, Adrien Guérou, Wolfram Kollatschny, Jarle Brinchmann, Lutz Wisotzki, 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), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Leiden Observatory [Leiden], Universiteit Leiden, Institut de recherche en astrophysique et planétologie (IRAP), European Southern Observatory (ESO), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut für Astrophysik [Göttingen], Georg-August-University = Georg-August-Universität Göttingen, Leibniz-Institut für Astrophysik Potsdam (AIP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden [Leiden], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Georg-August-University [Göttingen], Epinat, B, Contini, T, Finley, H, Boogaard, L, Guerou, A, Brinchmann, J, Carton, D, Michel-Dansac, L, Bacon, R, Cantalupo, S, Carollo, M, Hamer, S, Kollatschny, W, Krajnovic, D, Marino, R, Richard, J, Soucail, G, Weilbacher, P, and Wisotzki, L

Subjects
Active galactic nucleus, Absorption spectroscopy, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Galaxies: kinematics and dynamic, galaxies: groups: general, galaxies: high-redshift, Ionization, Galaxy group, 0103 physical sciences, Tidal force, galaxies: interactions, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: kinematics and dynamics, Line (formation), Physics, evolution, intergalactic medium, galaxies: high-redshift [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Galaxies: interaction, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: evolution
Abstract

We report the discovery of a 10^4 kpc^2 gaseous structure detected in [OII] in an over-dense region of the COSMOS-Gr30 galaxy group at z~0.725 thanks to deep MUSE Guaranteed Time Observations. We estimate the total amount of diffuse ionised gas to be of the order of (~5+-3)x10^10 Msun and explore its physical properties to understand its origin and the source(s) of the ionisation. The MUSE data allow the identification of a dozen of group members embedded in this structure from emission and absorption lines. We extracted spectra from small apertures defined for both the diffuse ionised gas and the galaxies. We investigated the kinematics and ionisation properties of the various galaxies and extended gas regions thanks to line diagnostics (R23, O32 and [OIII]/H\beta) available within the MUSE wavelength range. We compared these diagnostics to photo-ionisation models and shock models. The structure is divided in two kinematically distinct sub-structures. The most extended sub-structure of ionised gas is likely rotating around a massive galaxy and displays filamentary patterns linking some galaxies. The second sub-structure links another massive galaxy hosting an Active Galactic Nucleus to a low mass galaxy but also extends orthogonally to the AGN host disk over ~35 kpc. This extent is likely ionised by the AGN itself. The location of small diffuse regions in the R23 vs. O32 diagram is compatible with photo-ionisation. However, the location of three of these regions in this diagram (low O32, high R23) can also be explained by shocks, which is supported by their large velocity dispersions. One edge-on galaxy shares the same properties and may be a source of shocks. Whatever the hypothesis, the extended gas seems to be non primordial. We favour a scenario where the gas has been extracted from galaxies by tidal forces and AGN triggered by interactions between at least the two sub-structures., Comment: 21 pages, 12 figures, 3 tables, accepted for publication in A&A (27 October 2017)

Published
2018

47. Galactic winds with MUSE: A direct detection of Fe II* emission from a z 1.29 galaxy

Author

Hayley Finley, Nicolas Bouché, Thierry Contini, Benoît Epinat, Roland Bacon, Jarle Brinchmann, Sebastiano Cantalupo, Santiago Erroz-Ferrer, Raffaella Anna Marino, Michael Maseda, Johan Richard, Ilane Schroetter, Anne Verhamme, Peter M. Weilbacher, Martin Wendt, Lutz Wisotzki, Finley, H, Bouche, N, Contini, T, Epinat, B, Bacon, R, Brinchmann, J, Cantalupo, S, Erroz-Ferrer, S, Marino, R, Maseda, M, Richard, J, Schroetter, I, Verhamme, A, Weilbacher, P, Wendt, M, Wisotzki, L, 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
Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: formation, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Surface brightness, 010303 astronomy & astrophysics, ISM: jets and outflow, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, Ultraviolet: ISM, 010308 nuclear & particles physics, Star formation, Institut für Physik und Astronomie, Galaxies: evolution, Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, Galaxies: ISM, ISM: jets and outflows, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: starburst
Abstract

Emission signatures from galactic winds provide an opportunity to directly map the outflowing gas, but this is traditionally challenging because of the low surface brightness. Using deep observations (27 hours) of the Hubble Deep Field South from the Multi Unit Spectroscopic Explorer (MUSE) instrument, we identify signatures of an outflow in both emission and absorption from a spatially resolved galaxy at z = 1.29 with a stellar mass M* = 8 x 10^9 Msun, star formation rate SFR = 77 Msun/yr, and star formation rate surface brightness 1.6 Msun/kpc^2 within the [OII] half-light radius R_1/2,[OII] = 2.76 +- 0.17 kpc. From a component of the strong resonant MgII and FeII absorptions at -350 km/s, we infer a mass outflow rate that is comparable to the star formation rate. We detect non-resonant FeII* emission, at lambda 2626, 2612, 2396, and 2365, at 1.2-2.4-1.5-2.7 x 10^-18 egs s-1 cm-2 respectively. These flux ratios are consistent with the expectations for optically thick gas. By combining the four non-resonant FeII* emission lines, we spatially map the FeII* emission from an individual galaxy for the first time. The FeII* emission has an elliptical morphology that is roughly aligned with the galaxy minor kinematic axis, and its integrated half-light radius R_1/2,FeII* = 4.1 +- 0.4 kpc is 50% larger than the stellar continuum (R_1/2,* = 2.34 +- 0.17 kpc) or the [OII] nebular line. Moreover, the FeII* emission shows a blue wing extending up to -400 km/s, which is more pronounced along the galaxy minor kinematic axis and reveals a C-shaped pattern in a p-v diagram along that axis. These features are consistent with a bi-conical outflow., 13 pages, 6 figures, 4 tables, submitted to A&A - comments welcome

Published
2017

48. UBIQUITOUS GIANT Lyα NEBULAE AROUND the BRIGHTEST QUASARS at z ∼ 3.5 REVEALED with MUSE

Author

Jeremy Blaizot, C. Marcella Carollo, Elena Borisova, Joseph Caruana, Johan Richard, Raffaella Anna Marino, Lutz Wisotzki, Lorrie A. Straka, Tanya Urrutia, Simon J. Lilly, Monica L. Turner, Joop Schaye, Jarle Brinchmann, Edmund Christian Herenz, Sofia G. Gallego, Roland Bacon, A. Verhamme, Hayley Finley, Nicolas Bouché, Sebastiano Cantalupo, Borisova, E, Cantalupo, S, Lilly, S, Marino, R, Gallego, S, Bacon, R, Blaizot, J, Bouche, N, Brinchmann, J, Carollo, C, Caruana, J, Finley, H, Herenz, E, Richard, J, Schaye, J, Straka, L, Turner, M, Urrutia, T, Verhamme, A, and Wisotzki, L

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Power law, Luminosity, galaxies: high-redshift, quasars: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Nebula, cosmology: observation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Quasar, Multi Unit Spectroscopic Explorer, 13. Climate action, Space and Planetary Science, Intergalactic travel, intergalactic medium, Detection rate, quasars: emission line
Abstract

Direct Lyα imaging of intergalactic gas at $z\sim 2$ has recently revealed giant cosmological structures around quasars, e.g., the Slug Nebula. Despite their high luminosity, the detection rate of such systems in narrow-band and spectroscopic surveys is less than 10%, possibly encoding crucial information on the distribution of gas around quasars and the quasar emission properties. In this study, we use the MUSE integral-field instrument to perform a blind survey for giant $\mathrm{Ly}\alpha $ nebulae around 17 bright radio-quiet quasars at $3\lt z\lt 4$ that does not suffer from most of the limitations of previous surveys. After data reduction and analysis performed with specifically developed tools, we found that each quasar is surrounded by giant $\mathrm{Ly}\alpha $ nebulae with projected sizes larger than 100 physical kiloparsecs and, in some cases, extending up to 320 kpc. The circularly averaged surface brightness profiles of the nebulae appear to be very similar to each other despite their different morphologies and are consistent with power laws with slopes $\approx -1.8$. The similarity between the properties of all these nebulae and the Slug Nebula suggests a similar origin for all systems and that a large fraction of gas around bright quasars could be in a relatively “cold” (T ∼ 10(4 )K) and dense phase. In addition, our results imply that such gas is ubiquitous within at least 50 kpc from bright quasars at $3\lt z\lt 4$ independently of the quasar emission opening angle, or extending up to 200 kpc for quasar isotropic emission.

Published
2016

49. Muse Gas Flow and Wind (MEGAFLOW). I. First MUSE Results on Background Quasars

Author

Simon J. Lilly, Matthias Steinmetz, Ilane Schroetter, Johan Richard, Hayley Finley, Joop Schaye, Sebastiano Cantalupo, Roland Bacon, Martin Wendt, Nicolas Bouché, R. A. Marino, Kurt T. Soto, Lorrie A. Straka, Lutz Wisotzki, Thierry Contini, Roser Pello, Schroetter, I, Bouche, N, Wendt, M, Contini, T, Finley, H, Pello, R, Bacon, R, Cantalupo, S, Marino, R, Richard, J, Lilly, S, Schaye, J, Soto, K, Steinmetz, M, Straka, L, and Wisotzki, L

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, quasars: individual (SDSS J213748+001220, SDSS J215200+062516), 01 natural sciences, 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Spectrograph, Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Institut für Physik und Astronomie, Astronomy and Astrophysics, Quasar, Escape velocity, Multi Unit Spectroscopic Explorer, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), intergalactic medium, galaxies: evolution
Abstract

The physical properties of galactic winds are one of the keys to understand galaxy formation and evolution. These properties can be constrained thanks to background quasar lines of sight (LOS) passing near star-forming galaxies (SFGs). We present the first results of the MusE GAs FLOw and Wind (MEGAFLOW) survey obtained of 2 quasar fields which have 8 MgII absorbers of which 3 have rest-equivalent width greater than 0.8 \AA. With the new Multi Unit Spectroscopic Explorer (MUSE) spectrograph on the Very Large Telescope (VLT), we detect 6 (75$\%$) MgII host galaxy candidates withing a radius of 30 arcsec from the quasar LOS. Out of these 6 galaxy--quasar pairs, from geometrical arguments, one is likely probing galactic outflows, two are classified as "ambiguous", two are likely probing extended gaseous disks and one pair seems to be a merger. We focus on the wind$-$pair and constrain the outflow using a high resolution quasar spectra from Ultraviolet and Visual Echelle Spectrograph (UVES). Assuming the metal absorption to be due to gas flowing out of the detected galaxy through a cone along the minor axis, we find outflow velocities of the order of $\approx$ 150 km/s (i.e. smaller than the escape velocity) with a loading factor, $\eta =\dot M_{\rm out}/$SFR, of $\approx$ 0.7. We see evidence for an open conical flow, with a low-density inner core. In the future, MUSE will provide us with about 80 multiple galaxy$-$quasar pairs in two dozen fields., Comment: 20 pages, 16 figures, accepted for publication in ApJ

Published
2016

50. Possible Signatures of a Cold-Flow Disk from MUSE using a z=1 galaxy--quasar pair towards SDSSJ1422-0001

Author

Lutz Wisotzki, Philipp Richter, Wolfram Kollatschny, H. Finley, Sebastiano Cantalupo, Sebastian Kamann, Nicolas Bouché, Roland Bacon, Kurt T. Soto, Benoît Epinat, C. M. Carollo, Michael T. Murphy, Johan Richard, T. Contini, Lorrie A. Straka, Celine Peroux, Jarle Brinchmann, Simon J. Lilly, Martin Wendt, Joop Schaye, Crystal L. Martin, Ilane Schroetter, Bouche, N, Finley, H, Schroetter, I, Murphy, M, Richter, P, Bacon, R, Contini, T, Richard, J, Wendt, M, Kamann, S, Epinat, B, Cantalupo, S, Straka, L, Schaye, J, Martin, C, Peroux, C, Wisotzki, L, Soto, K, Lilly, S, Carollo, C, Brinchmann, J, and Kollatschny, W

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], Metallicity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Atomic, Physical Chemistry, Spectral line, Particle and Plasma Physics, 0103 physical sciences, galaxies: formation, Astrophysics::Solar and Stellar Astrophysics, Nuclear, 010303 astronomy & astrophysics, Stellar evolution, Astrophysics::Galaxy Astrophysics, evolution [galaxies], Physics, Very Large Telescope, individual [quasars], 010308 nuclear & particles physics, Star formation, Molecular, Astronomy and Astrophysics, Quasar, 16. Peace & justice, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, intergalactic medium, galaxies: evolution, quasars: individual (SDSS J142253.31-000149), Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Physical Chemistry (incl. Structural)
Abstract

We use a background quasar to detect the presence of circum-galactic gas around a $z=0.91$ low-mass star forming galaxy. Data from the new Multi Unit Spectroscopic Explorer (MUSE) on the VLT show that the host galaxy has a dust-corrected star-formation rate (SFR) of 4.7$\pm$0.2 Msun/yr, with no companion down to 0.22 Msun/yr (5 $\sigma$) within 240 kpc (30"). Using a high-resolution spectrum (UVES) of the background quasar, which is fortuitously aligned with the galaxy major axis (with an azimuth angle $\alpha$ of only $15^\circ$), we find, in the gas kinematics traced by low-ionization lines, distinct signatures consistent with those expected for a "cold flow disk" extending at least 12 kpc ($3\times R_{1/2}$). We estimate the mass accretion rate $\dot M_{\rm in}$ to be at least two to three times larger than the SFR, using the geometric constraints from the IFU data and the HI column density of $\log N_{\rm HI} \simeq 20.4$ obtained from a {\it HST}/COS NUV spectrum. From a detailed analysis of the low-ionization lines (e.g. ZnII, CrII, TiII, MnII, SiII), the accreting material appears to be enriched to about 0.4 $Z_\odot$ (albeit with large uncertainties: $\log Z/Z_\odot=-0.4~\pm~0.4$), which is comparable to the galaxy metallicity ($12+\log \rm O/H=8.7\pm0.2$), implying a large recycling fraction from past outflows. Blue-shifted MgII and FeII absorptions in the galaxy spectrum from the MUSE data reveal the presence of an outflow. The MgII and FeII doublet ratios indicate emission infilling due to scattering processes, but the MUSE data do not show any signs of fluorescent FeII* emission., Comment: 17 pages, 11 figures, in press (ApJ), minor edits after the proofs. Data available at http://muse-vlt.eu/science/j1422/

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