Spectral and photometric evolution of young stellar populations: The impact of gaseous emission at various metallicities

Anders, Peter; Alvensleben, Uta Fritze v.

doi:10.1051/0004-6361:20030151

Cited by 346 publications

(468 citation statements)

References 23 publications

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“…Bicker & Fritze-v. Alvensleben 2005). It has been shown to have a large impact, even on broad band luminosities and colors, during strong starbursts by Krüger et al (1995) (see also Anders & Fritze-v. Alvensleben 2003).…”

Section: Undisturbed Galaxiesmentioning

confidence: 98%

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

Alvensleben¹,

Bicker

2006

A&A

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We present evolutionary synthesis models for galaxies of spectral types Sa through Sd with starbursts of various strengths triggered at various redshifts and study their photometric evolution before, during, and after their bursts in a cosmological context. We find that bursts at high redshift, even very strong ones, only cause a small blueing of their intrinsically blue young parent galaxies. At lower redshift, in contrast, even small bursts cause a significant blueing of their intrinsically redder galaxies. While the burst phase is generally short, typically a few hundred Myr in normal-mass galaxies, the postburst stage with its red colors and, in particular the very red ones for early bursts at high redshift, lasts much longer, on the order of several Gyr. We find that, even without any dust, which in the postburst stage is not expected to play an important role anyway, models easily reach the colors of EROs in the redshift range z ∼ 2 through z ∼ 0.5 after starbursts at redshifts between 2 and 4. We therefore propose a third alternative for the ERO galaxies beyond the two established ones of passive galaxies vs. dusty starbursts: the dust-free post-(strong-)starbursts. A very first comparison of our models to HDF data with photometric redshifts shows that almost all of the outliers that could not be described with our chemically consistent models for undisturbed normal galaxy types E through Sd can now be explained very well. Galaxies in the redshift range from z ∼ 2.5 to z ∼ 0.5 that are redder, and in some cases much redder, than our reddest undisturbed model for a high-metallicity classical elliptical are well described by post-starburst models after starbursts at redshifts between 2 and 4. Galaxies bluer than our bluest low metallicity Sd model, most of which have redshifts lower than 1, are well explained by ongoing starbursts.

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Section: Undisturbed Galaxiesmentioning

confidence: 98%

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

Alvensleben¹,

Bicker

2006

A&A

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“…Non-zero Lyman continuum escape fraction will reduce the strength of optical nebular emission lines (see Inoue 2011 andSalmon et al 2015). We then use the tabulated line ratios between Hβ and the metal lines from Anders & Alvensleben (2003) to calculate the metal line fluxes for a metallicity of 0.2Z e . For templates with dust attenuation, we include the dust attenuation effects after adding nebular emission lines.…”

Section: Modeling Proceduresmentioning

confidence: 99%

SPITZER ULTRA FAINT SURVEY PROGRAM (SURFS UP). II. IRAC-DETECTED LYMAN-BREAK GALAXIES AT 6 ≲ z ≲ 10 BEHIND STRONG-LENSING CLUSTERS

Huang

Bradač

Lemaux

et al. 2016

ApJ

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We study the stellar population properties of the IRAC-detected 6  z  10 galaxy candidates from the Spitzer UltRa Faint SUrvey Program. Using the Lyman Break selection technique, we find a total of 17 galaxy candidates at 6  z  10 from Hubble Space Telescope images (including the full-depth images from the Hubble Frontier Fields program for MACS 1149 and MACS 0717) that have detections at signal-to-noise ratios  3 in at least one of the IRAC 3.6 and 4.5 μm channels. According to the best mass models available for the surveyed galaxy clusters, these IRAC-detected galaxy candidates are magnified by factors of ∼1.2-5.5. Due to the magnification of the foreground galaxy clusters, the rest-frame UV absolute magnitudes M 1600 are between −21.2 and −18.9 mag, while their intrinsic stellar masses are between 2×10 8 M e and 2.9×10 9 M e . We identify two Lyα emitters in our sample from the Keck DEIMOS spectra, one at z Lyα =6.76 (in RXJ 1347) and one at z Lyα =6.32 (in MACS 0454). We find that 4 out of 17 z  6 galaxy candidates are favored by z  1 solutions when IRAC fluxes are included in photometric redshift fitting. We also show that IRAC [3.6]-[4.5] color, when combined with photometric redshift, can be used to identify galaxies which likely have strong nebular emission lines or obscured active galactic nucleus contributions within certain redshift windows.

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“…14 Following this relation, we derived EW(Hα) for all considered redshifts. We also derived EWs for Hβ assuming case B recombination and the corresponding EWs for [O III] and [O II] by using the line ratios tabulated in Anders & Fritze-v. Alvensleben (2003). We Redshift distribution of the three galaxy samples considered in this work: a galaxy sample with spectroscopic redshifts in the GOODS-S field (filled gray; sample 1), a galaxy sample with well-established CANDELS photometric redshifts, also in GOODS-S (red line; sample 2), and a sample of simulated galaxies with known input redshifts (dashed line; sample 3).…”

Section: Samplementioning

confidence: 99%

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Bisigello

Caputi

Colina

et al. 2016

ApJS

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The determination of galaxy redshifts in the James Webb Space Telescope's (JWST) blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 μm and Mid Infrared Instrument (MIRI) at l m > 5.0 m. In this work we analyze the impact of choosing different combinations of NIRCam and MIRI broadband filters (F070W to F770W), as well as having ancillary data at l m < 0.6 m, on the derived photometric redshifts (z phot ) of a total of 5921 real and simulated galaxies, with known input redshifts z=0-10. We found that observations at l m < 0.6 m are necessary to control the contamination of high-z samples by low-z interlopers. Adding MIRI (F560W and F770W) photometry to the NIRCam data mitigates the absence of ancillary observations at l m < 0.6 m and improves the redshift estimation. At z=7-10, accurate z phot can be obtained with the NIRCam broadbands alone when  S N 10, but the z phot quality significantly degrades at  S N 5. Adding MIRI photometry with 1 mag brighter depth than the NIRCam depth allows for a redshift recovery of 83%-99%, depending on spectral energy distribution type, and its effect is particularly noteworthy for galaxies with nebular emission. The vast majority of NIRCam galaxies with [F150W]=29AB mag at z=7-10 will be detected with MIRI at [F560W, F770W] < 28 mag if these sources are at least mildly evolved or have spectra with emission lines boosting the mid-infrared fluxes.

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Spectral and photometric evolution of young stellar populations: The impact of gaseous emission at various metallicities

Cited by 346 publications

References 23 publications

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

SPITZER ULTRA FAINT SURVEY PROGRAM (SURFS UP). II. IRAC-DETECTED LYMAN-BREAK GALAXIES AT 6 ≲ z ≲ 10 BEHIND STRONG-LENSING CLUSTERS

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

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