scholarly journals The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: The Nature of the Faintest Dusty Star-forming Galaxies

2020 ◽  
Vol 901 (1) ◽  
pp. 79 ◽  
Author(s):  
Manuel Aravena ◽  
Leindert Boogaard ◽  
Jorge Gónzalez-López ◽  
Roberto Decarli ◽  
Fabian Walter ◽  
...  
Keyword(s):  
Star Forming ◽  
Hubble Ultra Deep Field

scholarly journals Clumpy Galaxies in the Early Universe

2006 ◽  
Vol 2 (S235) ◽  
pp. 376-380 ◽  
Author(s):  
Debra Meloy Elmegreen
Keyword(s):  
Star Formation ◽  
Early Universe ◽  
Spiral Galaxies ◽  
Star Forming ◽  
Wide Range ◽  
Thick Disks ◽  
Hubble Ultra Deep Field

AbstractClumpy galaxies are prominent in the early Universe. We present morphological and photometric properties of a wide range of galaxy types and their star-forming clumps in the Hubble Ultra Deep Field. Sizes, scale lengths, and scale heights suggest that galaxies grow by a factor of 2 fromz= 4 to the present, and that thick disks are present in the early Universe. The largest clumps of star formation are 107–109M⊙in different galaxies, much more massive than large star-forming complexes in local galaxies. Dissolved clumps may account for both the exponential disks and the early thick disks of spirals and proto-spiral galaxies.

scholarly journals The MUSE Hubble Ultra Deep Field Survey

2018 ◽  
Vol 617 ◽  
pp. A62 ◽  
Author(s):  
Anna Feltre ◽  
Roland Bacon ◽  
Laurence Tresse ◽  
Hayley Finley ◽  
David Carton ◽  
...  
Keyword(s):  
Spectral Energy Distribution ◽  
Gas Content ◽  
Spectral Energy ◽  
Distribution Fitting ◽  
Space Telescope ◽  
Star Forming ◽  
Neutral Gas ◽  
Near Ultraviolet ◽  
Hubble Ultra Deep Field ◽  
Stellar Masses

The physical origin of the near-ultraviolet Mg II emission remains an underexplored domain, unlike more typical emission lines that are detected in the spectra of star-forming galaxies. We explore the nebular and physical properties of a sample of 381 galaxies between 0.70 < z < 2.34 drawn from the MUSE Hubble Ultra Deep Survey. The spectra of these galaxies show a wide variety of profiles of the Mg II λλ2796, 2803 resonant doublet, from absorption to emission. We present a study on the main drivers for the detection of Mg II emission in galaxy spectra. By exploiting photoionization models, we verified that the emission-line ratios observed in galaxies with Mg II in emission are consistent with nebular emission from HII regions. From a simultaneous analysis of MUSE spectra and ancillary Hubble Space Telescope information through spectral energy distribution fitting, we find that galaxies with Mg II in emission have lower stellar masses, smaller sizes, bluer spectral slopes, and lower optical depth than those with absorption. This leads us to suggest that Mg II emission is a potential tracer of physical conditions that are not merely related to those of the ionized gas. We show that these differences in Mg II emission and absorption can be explained in terms of a higher dust and neutral gas content in the interstellar medium (ISM) of galaxies showing Mg II in absorption, which confirms the extreme sensitivity of Mg II to the presence of the neutral ISM. We conclude with an analogy between the Mg II doublet and the Ly α line that lies in their resonant nature. Further investigations with current and future facilities, including the James Webb Space Telescope, are promising because the detection of Mg II emission and its potential connection with Lyα could provide new insights into the ISM content in the early Universe.

scholarly journals The MUSE Hubble Ultra Deep Field Survey

2017 ◽  
Vol 608 ◽  
pp. A4 ◽  
Author(s):  
Michael V. Maseda ◽  
Jarle Brinchmann ◽  
Marijn Franx ◽  
Roland Bacon ◽  
Rychard J. Bouwens ◽  
...  
Keyword(s):  
Rest Frame ◽  
Optical Emission ◽  
Total Sample ◽  
Star Forming ◽  
Integral Field Spectroscopy ◽  
Ultraviolet C ◽  
Emission Line Galaxies ◽  
Hubble Ultra Deep Field ◽  
Statistical Sample ◽  
Dust Attenuation

The C III] λλ1907, 1909 emission doublet has been proposed as an alternative to Lyman-α in redshift confirmations of galaxies at z ≳ 6 since it is not attenuated by the largely neutral intergalactic medium at these redshifts and is believed to be strong in the young, vigorously star-forming galaxies present at these early cosmic times. We present a statistical sample of 17 C III]-emitting galaxies beyond z ~ 1.5 using ~30 h deep VLT/MUSE integral field spectroscopy covering 2 square arcminutes in the Hubble Deep Field South (HDFS) and Ultra Deep Field (UDF), achieving C III] sensitivities of ~ 2 × 10-17 erg s-1 cm-2 in the HDFS and ~ 7 × 10-18 erg s-1 cm-2 in the UDF. The rest-frame equivalent widths range from 2 to 19 Å. These 17 galaxies represent ~3% of the total sample of galaxies found between 1.5 ≲ z ≲ 4. They also show elevated star formation rates, lower dust attenuation, and younger mass-weighted ages than the general population of galaxies at the same redshifts. Combined with deep slitless grism spectroscopy from the HST/WFC3 in the UDF, we can tie the rest-frame ultraviolet C III] emission to rest-frame optical emission lines, namely [O III] λ5007, finding a strong correlation between the two. Down to the flux limits that we observe (~ 1 × 10-18 erg s-1 cm-2 with the grism data in the UDF), all objects with a rest-frame [O III] λλ4959, 5007 equivalent width in excess of 250 Å, the so-called extreme emission line galaxies, have detections of C III] in our MUSE data. More detailed studies of the C III]-emitting population at these intermediate redshifts will be crucial to understand the physical conditions in galaxies at early cosmic times and to determine the utility of C III] as a redshift tracer.

scholarly journals Dust attenuation in 2 < z < 3 star-forming galaxies from deep ALMA observations of the Hubble Ultra Deep Field

2018 ◽  
Vol 476 (3) ◽  
pp. 3991-4006 ◽  
Author(s):  
R J McLure ◽  
J S Dunlop ◽  
F Cullen ◽  
N Bourne ◽  
P N Best ◽  
...  
Keyword(s):  
Star Forming ◽  
Hubble Ultra Deep Field ◽  
Dust Attenuation

scholarly journals THE ABUNDANCE OF STAR-FORMING GALAXIES IN THE REDSHIFT RANGE 8.5-12: NEW RESULTS FROM THE 2012 HUBBLE ULTRA DEEP FIELD CAMPAIGN

2012 ◽  
Vol 763 (1) ◽  
pp. L7 ◽  
Author(s):  
Richard S. Ellis ◽  
Ross J. McLure ◽  
James S. Dunlop ◽  
Brant E. Robertson ◽  
Yoshiaki Ono ◽  
...  
Keyword(s):  
Field Campaign ◽  
Redshift Range ◽  
Star Forming ◽  
Hubble Ultra Deep Field

scholarly journals The MUSE Hubble Ultra Deep Field Survey

2017 ◽  
Vol 608 ◽  
pp. A8 ◽  
Author(s):  
Floriane Leclercq ◽  
Roland Bacon ◽  
Lutz Wisotzki ◽  
Peter Mitchell ◽  
Thibault Garel ◽  
...  
Keyword(s):  
High Redshift ◽  
Dark Matter Halo ◽  
Star Forming ◽  
Star Forming Regions ◽  
Size Evolution ◽  
Individual Star ◽  
Hubble Ultra Deep Field ◽  
Gas Accretion ◽  
Scale Length

We report the detection of extended Lyα haloes around 145 individual star-forming galaxies at redshifts 3 ≤ z ≤ 6 in the Hubble Ultra Deep Field observed with the Multi-Unit Spectroscopic Explorer (MUSE) at ESO-VLT. Our sample consists of continuum-faint (− 15 ≥ MUV ≥ −22) Lyα emitters (LAEs). Using a 2D, two-component (continuum-like and halo) decomposition of Lyα emission assuming circular exponential distributions, we measure scale lengths and luminosities of Lyα haloes. We find that 80% of our objects having reliable Lyα halo measurements show Lyα emission that is significantly more extended than the UV continuum detected by HST (by a factor ≈4 to >20). The median exponential scale length of the Lyα haloes in our sample is ≈4.5 kpc with a few haloes exceeding 10 kpc. By comparing the maximal detected extent of the Lyα emission with the predicted dark matter halo virial radii of simulated galaxies, we show that the detected Lyα emission of our selected sample of Lyα emitters probes a significant portion of the cold circum-galactic medium of these galaxies (>50% in average). This result therefore shows that there must be significant HI reservoirs in the circum-galactic medium and reinforces the idea that Lyα haloes are ubiquitous around high-redshift Lyα emitting galaxies. Our characterization of the Lyα haloes indicates that the majority of the Lyα flux comes from the halo (≈65%) and that their scale lengths seem to be linked to the UV properties of the galaxies (sizes and magnitudes). We do not observe a significant Lyα halo size evolution with redshift, although our sample for z> 5 is very small. We also explore the diversity of the Lyα line profiles in our sample and we find that the Lyα lines cover a large range of full width at half maximum (FWHM) from 118 to 512 km s-1. While the FWHM does not seem to be correlated to the Lyα scale length, most compact Lyα haloes and those that are not detected with high significance tend to have narrower Lyα profiles (<350 km s-1). Finally, we investigate the origin of the extended Lyα emission but we conclude that our data do not allow us to disentangle the possible processes, i.e. scattering from star-forming regions, fluorescence, cooling radiation from cold gas accretion, and emission from satellite galaxies.

scholarly journals The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field: CO Excitation and Atomic Carbon in Star-forming Galaxies at z = 1–3

2020 ◽  
Vol 902 (2) ◽  
pp. 109 ◽  
Author(s):  
Leindert A. Boogaard ◽  
Paul van der Werf ◽  
Axel Weiss ◽  
Gergö Popping ◽  
Roberto Decarli ◽  
...  
Keyword(s):  
Atomic Carbon ◽  
Star Forming ◽  
Hubble Ultra Deep Field

scholarly journals The MUSE Hubble Ultra Deep Field Survey

2018 ◽  
Vol 619 ◽  
pp. A27 ◽  
Author(s):  
Leindert A. Boogaard ◽  
Jarle Brinchmann ◽  
Nicolas Bouché ◽  
Mieke Paalvast ◽  
Roland Bacon ◽  
...  
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Analytical Models ◽  
High Signal ◽  
Noise Emission ◽  
Star Forming ◽  
Low Mass ◽  
Hydrodynamical Simulations ◽  
Hubble Ultra Deep Field ◽  
Intrinsic Scatter

Star-forming galaxies have been found to follow a relatively tight relation between stellar mass (M*) and star formation rate (SFR), dubbed the “star formation sequence”. A turnover in the sequence has been observed, where galaxies with M* <  1010 M⊙ follow a steeper relation than their higher mass counterparts, suggesting that the low-mass slope is (nearly) linear. In this paper, we characterise the properties of the low-mass end of the star formation sequence between 7 ≤ log M*[M⊙]  ≤  10.5 at redshift 0.11 <  z  <   0.91. We use the deepest MUSE observations of the Hubble Ultra Deep Field and the Hubble Deep Field South to construct a sample of 179 star-forming galaxies with high signal-to-noise emission lines. Dust-corrected SFRs are determined from Hβ λ4861 and Hα λ6563. We model the star formation sequence with a Gaussian distribution around a hyperplane between logM*, logSFR, and log(1 + z), to simultaneously constrain the slope, redshift evolution, and intrinsic scatter. We find a sub-linear slope for the low-mass regime where log SFR [M⊙yr−1] = 0.83+0.07−0.06 log M*[M⊙]+1.74+0.66−0.68 log(1 + z), increasing with redshift. We recover an intrinsic scatter in the relation of σintr = 0.44+0.05−0.04, dex, larger than typically found at higher masses. As both hydrodynamical simulations and (semi-)analytical models typically favour a steeper slope in the low-mass regime, our results provide new constraints on the feedback processes which operate preferentially in low-mass halos.

scholarly journals The MUSE Hubble Ultra Deep Field Survey

2020 ◽  
Vol 635 ◽  
pp. A82 ◽  
Author(s):  
Floriane Leclercq ◽  
Roland Bacon ◽  
Anne Verhamme ◽  
Thibault Garel ◽  
Jérémy Blaizot ◽  
...  
Keyword(s):  
Peak Velocity ◽  
High Redshift ◽  
Three Dimensional ◽  
Resonant Scattering ◽  
Spectral Signature ◽  
Star Forming ◽  
The Core ◽  
Velocity Shift ◽  
Spatially Resolved ◽  
Hubble Ultra Deep Field

We present spatially resolved maps of six individually-detected Lyman α haloes (LAHs) as well as a first statistical analysis of the Lyman α (Lyα) spectral signature in the circum-galactic medium of high-redshift star-forming galaxies (−17.5 >  MUV >  −21.5) using the Multi-Unit Spectroscopic Explorer. Our resolved spectroscopic analysis of the LAHs reveals significant intrahalo variations of the Lyα line profile. Using a three-dimensional two-component model for the Lyα emission, we measured the full width at half maximum (FWHM), the peak velocity shift, and the asymmetry of the Lyα line in the core and in the halo of 19 galaxies. We find that the Lyα line shape is statistically different in the halo compared to the core (in terms of width, peak wavelength, and asymmetry) for ≈40% of our galaxies. Similarly to object-by-object based studies and a recent resolved study using lensing, we find a correlation between the peak velocity shift and the width of the Lyα line both at the interstellar and circum-galactic scales. This trend has been predicted by radiative transfer simulations of galactic winds as a result of resonant scattering in outflows. While there is a lack of correlation between the spectral properties and the spatial scale lengths of our LAHs, we find a correlation between the width of the line in the LAH and the halo flux fraction. Interestingly, UV bright galaxies (MUV <  −20) show broader, more redshifted, and less asymmetric Lyα lines in their haloes. The most significant correlation found is for the FWHM of the line and the UV continuum slope of the galaxy, suggesting that the redder galaxies have broader Lyα lines. The generally broad and red line shapes found in the halo component suggest that the Lyα haloes are powered either by scattering processes through an outflowing medium, fluorescent emission from outflowing cold clumps of gas, or a mix of both. Considering the large diversity of the Lyα line profiles observed in our sample and the lack of strong correlation, the interpretation of our results is still broadly open and underlines the need for realistic spatially resolved models of the LAHs.

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