Template Ultraviolet to Near-Infrared Spectra of Star-forming Galaxies and Their Application to K-Corrections

Kinney, A. L.; Calzetti, Daniela; Bohlin, R. C.; Mcquade, Kerry; Storchi‐Bergmann, Thaisa; Schmitt, Henrique R.

doi:10.1086/177583

Cited by 919 publications

(1,207 citation statements)

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“…The galaxy NGC 1553 (Kinney et al 1996) is best reproduced by a t * = 1 Gyr model with an ∼ 11 Gyr old stellar population, a mean ISM metallicity of Z= 1.2 Z ⊙ and E(B-V) = 0.1.…”

Section: Comparision With Nearby Galaxiesmentioning

confidence: 97%

Untitled

Möller

Alvensleben

Fricke

et al. 2001

Astrophysics and Space Science

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Abstract.As a tool to interpret nearby and high redshift galaxy data from optical to K-band we present our chemically consistent spectrophotometric evolutionary synthesis models. These models take into account the increasing initial metallicity of successive stellar generations using recently published metallicity dependent stellar evolutionary tracks, stellar yields and model atmosphere spectra.The influence of the metallicity is analysed. Dust absorption is included on the basis of gas content and abundance as it varies with time and galaxy type. We compare our models with IUE template spectra and are able to predict UV fluxes for different spectral types. Combined with a cosmological model we obtain evolutionary and k-corrections for various galaxy types and show the differences to models using only solar metallicity input physics as a function of redshift, wavelength band and galaxy type.

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“…The galaxy NGC 1553 (Kinney et al 1996) is best reproduced by a t * = 1 Gyr model with an ∼ 11 Gyr old stellar population, a mean ISM metallicity of Z= 1.2 Z ⊙ and E(B-V) = 0.1.…”

Section: Comparision With Nearby Galaxiesmentioning

confidence: 97%

Untitled

Möller

Alvensleben

Fricke

et al. 2001

Astrophysics and Space Science

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“…(1), C color (m, z), was obtained by simulating galaxy SEDs from standard templates and applying the color criteria we used to select high-z galaxies. We used templates from Bruzual & Charlot (2003), Coleman et al (1980), Kinney et al (1996), Polletta et al (2007), and Silva et al (1998) and simulated 100 000 objects per bin of 0.25 mag in a redshift interval ranging from 0.0 to 10.00. We used filter transmissions and noise measured on each image as a function of magnitude to reproduce the photometric quality of real data.…”

Section: Completeness Of the Surveymentioning

confidence: 99%

“…Completeness of the color criteria used to select z ∼ 8 objects as a function of redshift and magnitude on the detection image. We simulated 100 000 galaxies per bin of 0.25 mag with a redshift ranging from 0 to 10 from standard templates (Bruzual & Charlot 2003;Coleman et al 1980;Kinney et al 1996;Polletta et al 2007;and Silva et al 1998). …”

Section: Completeness Of the Surveymentioning

confidence: 99%

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

Laporte

Streblyanska

Kim

et al. 2015

A&A

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Context. The Hubble Space Telescope (HST) Frontier Fields (HFFs) project started at the end of 2013 with the aim of providing extremely deep images of six massive galaxy clusters. One of the main goals of this program is to push several telescopes to their limits to provide the best current view of the earliest stages of the Universe. The analysis of the initial data has already demonstrated the huge capabilities of the program. Aims. We present a detailed analysis of z ∼ 8 objects behind the HFFs lensing cluster, MACSJ0416.1-2403, combining 0.3−1.6 µm imaging from HST, ground-based K s imaging from VLT HAWK-I, and 3.6 µm and 4.5 µm Spitzer Space Telescope. The images probe to 5σ depths of ≈29 AB for HST, 25.6 AB for HAWK-I, and ≈0.310 and 0.391 µJy at 3.6 and 4.5 µm, respectively. With these datasets, we assess the photometric properties of z ∼ 8 galaxies in this field, as well as their distribution in luminosity, to unprecedented sensitivity. Methods. We applied the classical Lyman break (LB) technique, which combines non detection criteria in bands blueward of the Lyman break at z ∼ 8 and color-selection in bands redward of the break. To avoid contamination by mid-z interlopers, we required a strong break between optical and near-infrared data. We determined the photometric properties of z ∼ 8 selected candidates using spectral energy distribution (SED)-fitting with standard library templates. The luminosity function at z ∼ 8 is computed using a Monte-Carlo method taking advantage of the SED-fitting results. A piece of cautionary information is gleaned from new deep optical photometry of a previously identified z ∼ 8 galaxy in this cluster, which is now firmly detected as a mid-z interloper with a strong ≈1.5 mag Balmer break (between F606W and F125W). Using the SED of this interloper, we estimated the contamination rate of our MACSJ0416.1−2403 sample, and that of previous samples in Abell 2744 that were based on HFF data, we highlight the dangers of pushing the LB technique too close to the photometry limits. Results. Our selection reliably recovers four objects with m F160W ranging from 26.0 to 27.9 AB that are located in modestamplification regions (µ < 2.4). Two of the objects display a secondary break between the IRAC 3.6 µm and 4.5 µm bands, which could be associated to the Balmer break or emission lines at z ∼ 8. The SED-fitting analysis suggests that all of these objects favor high-z solutions with no reliable secondary solutions. The candidates generally have star formation rates around ∼10 M /yr and sizes ranging from 0.2 to 0.5 kpc, which agrees well with previous observations and expectations for objects in the early Universe. The sample size and luminosity distribution are consistent with previous findings.

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“…The expected colours for a population of galaxies were calculated using the galaxy spectral templates by Kinney et al (1996). This library consists of ten SEDs averaged from integrated spectra of local galaxies ranging in wavelength from 125 nm to 1000 nm.…”

Section: Location Of Other Astrophysical Objects In the Diagrammentioning

confidence: 99%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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Abstract.We report the discovery of the optical and near-infrared counterparts to GRB 001011. The GRB 001011 error box determined by Beppo-SAX was simultaneously imaged in the near-infrared by the 3.58-m New Technology Telescope and in the optical by the 1.54-m Danish Telescope ∼8 hr after the gamma-ray event. Here we implement the colour-colour discrimination technique proposed by Rhoads (2001) and extend it using near-IR data as well. We present the results provided by an automatic colour-colour discrimination pipe-line developed to discern the different populations of objects present in the GRB 001011 error box. Our software revealed three candidates based on single-epoch images. Second-epoch observations carried out ∼3.2 days after the burst revealed that the most likely candidate had faded, thus identifying it with the counterpart to the GRB. In deep R-band images obtained 7 months after the burst a faint (R = 25.38 ± 0.25) elongated object, presumably the host galaxy of GRB 001011, was detected at the position of the afterglow. The GRB 001011 afterglow is the first discovered with the assistance of colour-colour diagram techniques. We discuss the advantages of using this method and its application to error boxes determined by future missions.

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Template Ultraviolet to Near-Infrared Spectra of Star-forming Galaxies and Their Application to K-Corrections

Cited by 919 publications

References 0 publications

Untitled

Untitled

Frontier Fields: Combining HST, VLT, andSpitzerdata to explore thez~ 8 Universe behind the lensing cluster MACSJ0416.1−2403

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

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