Local Lyman Break Galaxy Analogs: The Impact of Massive Star-Forming Clumps on the Interstellar Medium and the Global Structure of Young, Forming Galaxies

Overzier, Roderik; Heckman, Timothy M.; Tremonti, Christy; Armus, L.; Basu-Zych, Antara; Gonçalves, T. S.; Rich, R. Michael; Martin, D. Christopher; Ptak, A.; Schiminovich, David; Ford, H. C.; Madore, Barry F.; Seibert, Mark

doi:10.1088/0004-637x/706/1/203

Cited by 116 publications

(282 citation statements)

References 152 publications

(211 reference statements)

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“…The host galaxy of the QSO was not detected by ALMA (Willott et al 2013), putting tight constraints on the SFR in the QSO host. It may therefore be possible that the QSO itself is in a low mass halo and therefore does not reside in a high density peak in the early Universe (Overzier et al 2009). …”

Section: Physical Interpretationmentioning

confidence: 99%

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No Ly α emitters detected around a QSO at z = 6.4: Suppressed by the QSO?

Goto

Utsumi

Kikuta

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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Understanding how QSO's UV radiation affects galaxy formation is vital to our understanding of reionization era. Using a custom made narrow-band filter, N B906, on Subaru/SuprimeCam, we investigated the number density of Lyα emitters (LAE) around a QSO at z=6.4. To date, this is the highest redshift narrow-band observation, where LAEs around a luminous QSO are investigated. Due to the large field-of-view of Suprime-Cam, our survey area is ∼5400 cMpc 2 , much larger than previously studies at z=5.7 (∼200 cMpc 2 ).In this field, we previously found a factor of 7 overdensity of Lyman break galaxies (LBGs). Based on this, we expected to detect ∼100 LAEs down to N B906=25 ABmag. However, our 6.4 hour exposure found none. The obtained upper limit on the number density of LAEs is more than an order lower than the blank fields. Furthermore, this lower density of LAEs spans a large scale of 10 pMpc across. A simple argument suggests a strong UV radiation from the QSO can suppress star-formation in halos with M vir < 10 10 M ⊙ within a pMpc from the QSO, but the deficit at the edge of the field (5 pMpc) remains to be explained.

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Section: Physical Interpretationmentioning

confidence: 99%

“…Such massive hales are theoretically expected to hold many massive galaxies, and evolve into present-day massive clusters although with a significant scatter (e.g., Springel et al 2005;Overzier et al 2009).…”

Section: Introductionmentioning

confidence: 99%

No Ly α emitters detected around a QSO at z = 6.4: Suppressed by the QSO?

Goto

Utsumi

Kikuta

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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“…The clumpy fraction ( f clumpy ; clumpy galaxies/SF galaxies) have been investigated for different redshift and mass ranges Overzier et al 2009;Puech 2010;Guo et al 2012Guo et al , 2015Wuyts et al 2012;Murata et al 2014;Tadaki et al 2014). Despite the already mentioned differences in the clump definition, a remarkable agreement has been reached, concluding that f clumpy increases with redshift.…”

Section: Comparison With the Literature At This Redshiftmentioning

confidence: 99%

Starburst galaxies in the COSMOS field: clumpy star-formation at redshift 0 <z< 0.5

Hinojosa-Goñi

Muñoz–Tuñón

Méndez-Abreu

2016

A&A

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Context. At high redshift, starburst galaxies present irregular morphologies with 10−20% of their star formation occurring in giant clumps. These clumpy galaxies are considered the progenitors of local disk galaxies. To understand the properties of starbursts at intermediate and low redshift, it is fundamental to track their evolution and the possible link with the systems at higher z. Aims. We present an extensive, systematic, and multiband search and analysis of the starburst galaxies at redshift (0 < z < 0.5) in the COSMOS field, as well as detailed characteristics of their star-forming clumps by using Hubble Space Telescope/Advance Camera for Surveys (HST/ACS) images. Methods. The starburst galaxies are identified using a tailor-made intermediate-band color excess selection, tracing the simultaneous presence of Hα and [OIII] emission lines in the galaxies. Our methodology uses previous information from the zCOSMOS spectral database to calibrate the color excess as a function of the equivalent width of both spectral lines. This technique allows us to identify 220 starburst galaxies at redshift 0 < z < 0.5 using the SUBARU intermediate-band filters. Combining the high spatial resolution images from the HST/ACS with ground-based multi-wavelength photometry, we identify and parametrize the star-forming clumps in every galaxy. Their principal properties, sizes, masses, and star formation rates are provided. Results. The mass distribution of the starburst galaxies is remarkably similar to that of the whole galaxy sample with a peak around M/M ∼ 2 × 10 8 and only a few galaxies with M/M > 10 10 . We classify galaxies into three main types, depending on their HST morphology: single knot (Sknot), single star-forming knot plus diffuse light (Sknot+diffuse), and multiple star-forming knots (Mknots/clumpy) galaxy. We found a fraction of Mknots/clumpy galaxy f clumpy = 0.24 considering out total sample of starburst galaxies up to z ∼ 0.5. The individual star-forming knots in our sample follows the same L(Hα) vs. size scaling relation as local giant HII regions. However, they slightly differ from the one provided using samples at high redshift. This result highlights the importance of spatially resolving the star-forming regions for this kind of study. Star-forming clumps in the central regions of Mknots galaxies are more massive, and present higher star formation rates, than those in the outskirts. This trend is less clear when we consider either the mass surface density or surface star formation rate. Sknot galaxies do show properties similar to both dwarf elliptical and irregulars in the surface brightness (µ) versus M host diagram in the B-band, and to spheroidals and ellipticals in the µ versus M host diagram in the V-band. Conclusions. The properties of our star-forming knots in Sknot+diffuse and Mknots/clumpy galaxies support the predictions of recent numerical simulations claiming that they have been produced by violent disk instabilities. We suggest that the evolution of these knots means that large and m...

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“…Studies of LBAs also point to mergers as likely triggers of the starbursts, which seem to give LBGs their characteristic properties (Gonçalves et al 2010;Overzier et al 2008Overzier et al , 2009). In galaxy mergers, the detailed dynamical interplay of dark matter, stellar components, cold gas inflow, and feedback from triggered star formation determine the progress of the starburst and how long it can carry on before being quenched.…”

Section: Introductionmentioning

confidence: 99%

Kinematics of Haro 11: The miniature Antennae

Östlin

Marquart

Cumming

et al. 2015

A&A

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Luminous blue compact galaxies are among the most active galaxies in the local Universe in terms of their star formation rate per unit mass. They are rare at the current cosmic epoch, but were more abundant in the past and may be seen as the local analogues of higher red shift Lyman break galaxies. Studies of their kinematics is key to understanding what triggers their unusually active star formation. In this work, we investigate the kinematics of stars and ionised gas in Haro 11, one of the most luminous blue compact galaxies in the local Universe. Previous works have indicated that many of these galaxies may be triggered by galaxy mergers. We have employed Fabry-Perot interferometry, long-slit spectroscopy, and integral field unit (IFU) spectroscopy to explore the kinematics of Haro 11. We target the near-infrared calcium triplet, and use cross-correlation and penalised pixel fitting techniques to derive the stellar velocity field and velocity dispersion. We analyse ionised gas through emission lines from hydrogen, [O ], and [S ]. When spectral resolution and signal to noise allows, we investigate the line profile in detail and identify multiple velocity components when present. The spectra reveal a complex velocity field whose components, both stellar and gaseous, we attempt to disentangle. We find that to first order, the velocity field and velocity dispersions derived from stars and ionised gas agree. Hence the complexities reveal real dynamical disturbances providing further evidence for a merger in Haro 11. Through decomposition of emission lines, we find evidence for kinematically distinct components, for instance, a tidal arm. The ionised gas velocity field can be traced to large galactocentric radii, and shows significant velocity dispersion even far out in the halo. If interpreted as virial motions, this indicates that Haro 11 may have a mass of ∼10 11 M . Haro 11 shows many resemblances with the famous Antennae galaxies both morphologically and kinematically, but it is much denser, which is the likely explanation for the higher star formation efficiency in Haro 11.

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Local Lyman Break Galaxy Analogs: The Impact of Massive Star-Forming Clumps on the Interstellar Medium and the Global Structure of Young, Forming Galaxies

Cited by 116 publications

References 152 publications

No Ly α emitters detected around a QSO at z = 6.4: Suppressed by the QSO?

No Ly α emitters detected around a QSO at z = 6.4: Suppressed by the QSO?

Starburst galaxies in the COSMOS field: clumpy star-formation at redshift 0 <z< 0.5

Kinematics of Haro 11: The miniature Antennae

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