LYMAN CONTINUUM ESCAPE FRACTION OF STAR-FORMING DWARF GALAXIES AT z ∼ 1

Rutkowski, Michael J.; Scarlata, Claudia; Haardt, Francesco; Siana, Brian; Henry, Alaina; Rafelski, Marc; Hayes, Matthew; Salvato, M.; Pahl, Anthony; Mehta, Vihang; Beck, Mélanie; Malkan, Matthew A.; Teplitz, Harry I.

doi:10.3847/0004-637x/819/1/81

Cited by 85 publications

(114 citation statements)

References 103 publications

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“…Studies with the HUT (Leitherer et al 1995) and the HST SBC (e.g., Malkan et al 2003;Siana et al 2010) do not detect escaping LyC. Large archival studies of LyC emission from SFGs (Cowie et al 2009) and Hα-selected emission line galaxies (Rutkowski et al 2016) have generally reported non-detections, likely indicating that the strong star formation may be conducive to LyC escape, but does not guarantee it. Until recently, few LyC leakers were known; local starbursts Tol 0440-381, Tol 1247-232, Mrk 54, and Haro11 (e.g., Leitherer et al 2016;Puschnig et al 2016) and, at z2, fewer than ∼10, UV-selected SFGs (e.g., de Mostardi et al 2016;Smith et al 2016).…”

Section: Introductionmentioning

confidence: 98%

The Lyman Continuum Escape Fraction of Emission Line-selected z ∼ 2.5 Galaxies Is Less Than 15%

Rutkowski

Scarlata

Henry

et al. 2017

ApJL

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Recent work suggests that strong emission line, star-forming galaxies (SFGs) may be significant Lyman continuum leakers. We combine archival Hubble Space Telescope broadband ultraviolet and optical imaging (F275W and F606W, respectively) with emission line catalogs derived from WFC3 IR G141 grism spectroscopy to search for escaping Lyman continuum (LyC) emission from homogeneously selected z∼2. ELGs, f esc 14.0%. Our observations are not deep enough to detect f esc ∼10% typical of low-redshift Lyman continuum emitters. However, we find that this population represents a small fraction of the star-forming galaxy population at z∼2. Thus, unless the number of extreme emission line galaxies grows substantially to z6, such galaxies may be insufficient for reionization. Deeper survey data in the rest-frame ionizing UV will be necessary to determine whether strong line ratios could be useful for pre-selecting LyC leakers at high redshift.

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Section: Introductionmentioning

confidence: 98%

The Lyman Continuum Escape Fraction of Emission Line-selected z ∼ 2.5 Galaxies Is Less Than 15%

Rutkowski

Scarlata

Henry

et al. 2017

ApJL

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“…The two effects, however, may be negligible for our low-mass galaxies. The Lyman continuum escape fraction is less than 2% for galaxies at z ∼ 1 (Siana et al 2007(Siana et al , 2010Rutkowski et al 2016). And the dust absorption would preferentially affect massive (and hence dustier) galaxies rather than low-mass systems.…”

Section: Effects Of Dust Extinction Correctionmentioning

confidence: 99%

THE BURSTY STAR FORMATION HISTORIES OF LOW-MASS GALAXIES AT 0.4 < z < 1 REVEALED BY STAR FORMATION RATES MEASURED FROM Hβ AND FUV

Guo

Rafelski

Faber

et al. 2016

ApJ

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We investigate the burstiness of star formation histories (SFHs) of galaxies at 0.4<z<1 by using the ratio of star formation rates (SFRs) measured from Hβ and FUV (1500 Å) (Hβ-to-FUV ratio). Our sample contains 164 galaxies down to stellar mass (M * ) of 10 8.5 M e in the CANDELS GOODS-N region, where Team Keck Redshift Survey Keck/DEIMOS spectroscopy and Hubble Space Telescope/WFC3 F275W images from CANDELS and Hubble Deep UV Legacy Survey are available. When the ratio of Hβ-and FUV-derived SFRs is measured, dust extinction correction is negligible (except for very dusty galaxies) with the Calzetti attenuation curve. The Hβ-to-FUV ratio of our sample increases with M * and SFR. The median ratio is ∼0.7 at M * ∼10 8.5 M e (or SFR∼0.5 M e yr −1 ) and increases to ∼1 at M * ∼10 10 M e (or SFR∼10 M e yr −1 ). At M * <10 9.5 M e , our median Hβ-to-FUV ratio is lower than that of local galaxies at the same M * , implying a redshift evolution. Bursty SFH on a timescale of a few tens of megayears on galactic scales provides a plausible explanation for our results, and the importance of the burstiness increases as M * decreases. Due to sample selection effects, our Hβ-to-FUV ratio may be an upper limit of the true value of a complete sample, which strengthens our conclusions. Other models, e.g., non-universal initial mass function or stochastic star formation on star cluster scales, are unable to plausibly explain our results.

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“…On the other hand, recent estimates of the Lyman continuum escape fraction for low mass star-forming galaxies at z ∼ 1 based on HST grism spectroscopy plus GALEX FUV indicate escape fractions of less than 2% (Rutkowski et al 2016), which would not be sufficient to illuminate external gas.…”

Section: Associated H I Gasmentioning

confidence: 99%

Hubble Space Telescope Observations of Accretion-Induced Star Formation in the Tadpole Galaxy Kiso 5639

Elmegreen

Elmegreen²,

Alméida

et al. 2016

ApJ

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The tadpole galaxy Kiso 5639 has a slowly rotating disk with a drop in metallicity at its star-forming head, suggesting that star formation was triggered by the accretion of metal-poor gas. We present multi-wavelength Hubble Space Telescope Wide Field Camera 3 images of UV through I band plus Hα to search for peripheral emission and determine the properties of various regions. The head has a mass in young stars of~ M 10 6 and an ionization rate of6.4 10 51 s −1 , equivalent to ∼2100 O9-type stars. There are four older star-forming regions in the tail, and an underlying disk with a photometric age of ∼1 Gyr. The mass distribution function of 61 star clusters is a power law with a slope of −1.73±0.51. Fourteen young clusters in the head are more massive than, suggesting a clustering fraction of 30%-45%. Wispy filaments of Hα emission and young stars extend away from the galaxy. Shells and holes in the head H II region could be from winds and supernovae. Gravity from the disk should limit the expansion of the H II region, although hot gas might escape through the holes. The star formation surface density determined from Hα in the head is compared to that expected from likely pre-existing and accreted gas. Unless the surface density of the accreted gas is a factor of ∼3 or more larger than what was in the galaxy before, the star formation rate has to exceed the usual Kennicutt-Schmidt rate by a factor of 5.

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LYMAN CONTINUUM ESCAPE FRACTION OF STAR-FORMING DWARF GALAXIES AT z ∼ 1

Cited by 85 publications

References 103 publications

The Lyman Continuum Escape Fraction of Emission Line-selected z ∼ 2.5 Galaxies Is Less Than 15%

The Lyman Continuum Escape Fraction of Emission Line-selected z ∼ 2.5 Galaxies Is Less Than 15%

THE BURSTY STAR FORMATION HISTORIES OF LOW-MASS GALAXIES AT 0.4 < z < 1 REVEALED BY STAR FORMATION RATES MEASURED FROM Hβ AND FUV

Hubble Space Telescope Observations of Accretion-Induced Star Formation in the Tadpole Galaxy Kiso 5639

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