Did galaxy assembly and supermassive black-hole growth go hand-in-hand?

Windhorst, Rogier A.; Cohen, Seth H.; Straughn, Amber N.; Ryan, Russell E.; Hathi, N. P.; Jansen, Rolf A.; Koekemoer, Anton M.; Pirzkal, Norbert; Xu, C. K.; Mobasher, Bahram; Malhotra, Sangeeta; Strolger, L.; Rhoads, James E.

doi:10.1016/j.newar.2006.06.072

Cited by 10 publications

(9 citation statements)

References 38 publications

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“…In particular, star-forming dwarf galaxies with cometary morphology are commonly observed in high-redshift surveys, such as the Hubble Deep Field (HDF; e.g. van den Bergh et al 1996; ⋆ E-mail: plagos@astro.up.pt Straughn et al 2006;Windhorst et al 2006). This cometary morphology has been interpreted for high redshift galaxies in the HDF as: 1) the result of weak tidal interactions; 2) gravitational instabilities in gas-rich and turbulent galactic disks in the process of forming (Bournaud & Elmegreen 2009) and 3) stream-like accretion of metal-poor gas from the cosmic web (e.g.…”

Section: Introductionmentioning

confidence: 99%

Detecting metal-poor gas accretion in the star-forming dwarf galaxies UM 461 and Mrk 600

Lagos

Scott

Nigoche-Netro³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Using VIMOS-IFU observations, we study the interstellar medium (ISM) of two star-forming dwarf galaxies, UM 461 and Mrk 600. Our aim was to search for the existence of metallicity inhomogeneities that might arise from infall of nearly pristine gas feeding ongoing localized star-formation. The IFU data allowed us to study the impact of external gas accretion on the chemical evolution as well as the ionised gas kinematics and morphologies of these galaxies. Both systems show signs of morphological distortions, including cometary-like morphologies. We analysed the spatial variation of 12 + log(O/H) abundances within both galaxies using the direct method (T e ), the widely applied HII-CHI-mistry code, as well as by employing different standard calibrations. For UM 461 our results show that the ISM is fairly well mixed, at large scales, however we find an off-centre and low-metallicity region with 12 + log(O/H) < 7.6 in the SW part of the brightest H ii region, using the direct method. This result is consistent with the recent infall of a low mass metal-poor dwarf or H i cloud into the region now exhibiting the lowest metallicity, which also displays localized perturbed neutral and ionized gas kinematics. Mrk 600 in contrast, appears to be chemically homogeneous on both large and small scales. The intrinsic differences in the spatially resolved properties of the ISM in our analysed galaxies are consistent with these systems being at different evolutionary stages.

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Section: Introductionmentioning

confidence: 99%

Detecting metal-poor gas accretion in the star-forming dwarf galaxies UM 461 and Mrk 600

Lagos

Scott

Nigoche-Netro³

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Tadpole galaxies as a subset have proven interesting to study in part due to the relative ease of selecting their morphologies; i.e., a bright star-forming "head" offset to a diffuse "tail." There are several possibilities of the origin of the morphology, including edge-on disks with a large star-forming region at one end, asymmetrical ring galaxies viewed edge-on (Elmegreen & Elmegreen 2010), or some type of interaction or assembly process (Straughn et al 2006, Windhorst et al 2006, Rhoads et al 2005. In the deepest imaging available, tadpoles at moderate redshift represent somewhere between 6-10% of galaxies depending on size cuts (Straughn et al 2006, Elmegreen et al 2005.…”

Section: Introductionmentioning

confidence: 99%

A Multiwavelength Study of Tadpole Galaxies in the Hubble Ultra Deep Field

Straughn

Voyer

Eufrasio

et al. 2015

ApJ

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Multiwavelength data are essential in order to provide a complete picture of galaxy evolution and to inform studies of galaxies' morphological properties across cosmic time. Here we present results of a multiwavelength investigation of the morphologies of "tadpole" galaxies at intermediate redshift (0.314 < z < 3.175) in the Hubble Ultra Deep Field. These galaxies were previously selected from deep Hubble Space Telescope (HST) F775W data based on their distinct asymmetric knot-plus-tail morphologies (Straughn et al. 2006). Here we use deep Wide Field Camera 3 near-infrared imaging in addition to the HST optical data in order to study the rest-frame UV/optical morphologies of these galaxies across the redshift range 0.3

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“…This, together with the low ( > ∼ 1 Gyr) luminosity-weighted age of XBCDs, suggests that most of their stellar mass has formed in the past 1−3 Gyr (Papaderos et al 2008). Interestingly, a significant fraction (≥10%) of unevolved high-redshift galaxies in the Hubble Deep Field also show cometary (also referred to as "tadpole") morphology (van den Bergh et al 1996;Elmegreen et al 2005Elmegreen et al , 2007Straughn et al 2006;Windhorst et al 2006). …”

Section: Introductionmentioning

confidence: 99%

On the properties of the interstellar medium in extremely metal-poor blue compact dwarf galaxies

Lagos

Papaderos

Gomes

et al. 2014

A&A

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Aims. The main goal of this study is to carry out a spatially resolved investigation of the warm interstellar medium (ISM) in the extremely metal-poor blue compact dwarf (BCD) galaxy HS 2236+1344. Special emphasis is laid on analysis of the spatial distribution of chemical abundances, emission-line ratios, and the kinematics of the ISM, and to the recent star-forming (SF) activity in this galaxy. Methods. This study is based on optical integral field unit spectroscopy data from Gemini Multi-Object Spectrograph (GMOS) at the Gemini North telescope and archival Sloan Digital Sky Survey (SDSS) images. The galaxy was observed at medium spectral resolution over the spectral range from ∼4300 Å to 7300 Å. The data were obtained in two different positions across the galaxy, obtaining a total 4 × 8 field that encompasses most of its ISM.Results. Emission-line maps and broad-band images obtained in this study indicate that HS 2236+1344 hosts three giant H ii regions (GH iiRs). Our data also reveal some faint curved features in the BCD periphery that might be due to tidal perturbations or expanding ionized-gas shells. The ISM velocity field shows systematic gradients along the major axis of the BCD, with its southeastern and northwestern half differing by ∼80 km s −1 in their recessional velocity over the field of view. The Hα and Hβ equivalent-width distribution in the central part of HS 2236+1344 is consistent with a very young (∼3 Myr) burst. Our surface photometry analysis reveals an underlying low surface brightness component with moderately red colors, which suggest that the galaxy has undergone previous star formation. We derive an integrated oxygen abundance of 12 + log(O/H) = 7.53 ± 0.06 and a nitrogen-to-oxygen ratio of log(N/O) = −1.57 ± 0.19. Our results are consistent, within the uncertainties, with a homogeneous distribution of oxygen and nitrogen within the ISM of the galaxy. The high-ionization He ii λ4686 emission line is detected only in the central part of HS 2236+1344. Similar to many BCDs with He ii λ4686 emission, HS 2236+1344 shows no Wolf-Rayet (WR) bump.

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Did galaxy assembly and supermassive black-hole growth go hand-in-hand?

Cited by 10 publications

References 38 publications

Detecting metal-poor gas accretion in the star-forming dwarf galaxies UM 461 and Mrk 600

Detecting metal-poor gas accretion in the star-forming dwarf galaxies UM 461 and Mrk 600

A Multiwavelength Study of Tadpole Galaxies in the Hubble Ultra Deep Field

On the properties of the interstellar medium in extremely metal-poor blue compact dwarf galaxies

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