Gravitationally lensed high redshift galaxies in the field of 1E0657-56

Mehlert, D.; Seitz, S.; Saglia, R. P.; Appenzeller, I.; Bender, Ralf; Fricke, K. J.; Hoffman, T.; Hopp, U.; Kudritzki, R. P.; Pauldrach, A. W. A.

doi:10.1051/0004-6361:20011286

Cited by 29 publications

(58 citation statements)

References 27 publications

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“…'I\1cker, Tananbaum, & Remillard (1995 did CCD imaging of the field and discovered the cluster as well as a 12" luminous arc. Mehlert, et al (2001) spectroscopically confirmed the object as an LBG.…”

Section: The Bullet Clustermentioning

confidence: 78%

“…in tlw field of lE 0657-56, colloquially known as the Bullet Cluster. Mehlert, et al (2001) spectroscopically confirmed it as an LBG. The Bullet Cluster is actually at least two clusters in the process of merging and is one of the hottest X-ray clusters known (Tucker, et al 1998).…”

Section: The Bullet Clustermentioning

confidence: 80%

“…This is well below the limit where the SDSS photometry is reliable. The Mehlert, et al (2001) image is from the VLT and has 0.80" seeing in the R band which is considerably better than the median SDSS seeing of 1.43". The LBG has a length of 14" and width of 1.8" so the surface brightness is low.…”

Section: The Bullet Clustermentioning

confidence: 90%

“…There is also a strong correlation of C IV with redshift which Mehlert, et al (2001) interpret as an increase in metallicity with the age of the universe.…”

Section: The Bullet Clustermentioning

confidence: 95%

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Galaxy Evolution Insights from Spectral Modeling of Large Data Sets from the Sloan Digital Sky Survey

Hoversten¹

2007

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This thesis centers on the use of spectral modeling techniques on data from the Sloan Digital Sky Survey (SDSS) to gain new insights into current questions in galaxy evolution. The SDSS provides a large, uniform, high quality data set which can be exploited in a number of ways. One avenue pursued here is to use the large sample size to measure precisely the mean properties of galaxies of increasingly narrow parameter ranges. The other route taken is to look for rare objects which open up for exploration new areas in galaxy parameter space.The crux of this thesis is revisiting the classical Kennicutt method for inferring the stellar initial mass function (Il\IIF) from the integrated light propertie8 of galaxies. A large data set ('"'-' 10 5 galaxies) from the SDSS DR4 is combined with more in-depth modeling and quantitative statistical analysis to search for 8ystematic IMF variations as a function of galaxy luminosity. Galaxy Ha equivalent widths are compared to a broadband color index to constrain the IMF. It is found that for the sample as a whole the best fitting IMF power law slope above 0.5 M 0 is r = 1.5 ± 0.1 with the error dominated by systematics. Galaxies brighter than around M,., 0 . 1 = -20 ii (including galaxies like the :Milky Way which has fvlr,o. 1 ,....., -21) are well fit by a universal r , . . . . . , 1.4 INIF, similar to the classical Salpeter slope, and smooth, exponential star formation histories (SFI-I). Fainter galaxies prefer steeper IrvIFs and the quality of the fits reveal that for these galaxies a universal IlVIF with smooth SFI-Is is actually a poor assumption.Related projects are also pursued. A targeted photometric search is conducted for strongly lensed Lyman break galaxies (LBG) similar to MS1512-cB58.The evolution of the photometric selection technique is described as are the results of spectroscopic follow-up of the best targets. The serendipitous discovery of two interesting blue compact dwarf galaxies is reported. These galaxies were identified by their extremely weak ( < 150) [NII] ,\6584 to Ha emission line ratios. Abundance analysis from emission line fluxes reveals that these galaxies have gas phase oxygen abundances 12 + log(O/I-I),....., 7.7 to 7.9, not remarkably low, and near infrared imaging detects an old stellar population. However the measured nitrogen to oxygen ratios log(N/O) < 1.7 are anomalously low for blue compact dwarf galaxies. These objects may be useful for understanding the chemical evolution of nitrogen.

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Section: The Bullet Clustermentioning

confidence: 78%

Section: The Bullet Clustermentioning

confidence: 80%

Section: The Bullet Clustermentioning

confidence: 90%

“…There is also a strong correlation of C IV with redshift which Mehlert, et al (2001) interpret as an increase in metallicity with the age of the universe.…”

Section: The Bullet Clustermentioning

confidence: 95%

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Galaxy Evolution Insights from Spectral Modeling of Large Data Sets from the Sloan Digital Sky Survey

Hoversten¹

2007

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“…In the following section, we illustrate a method to help in the robust identification and/or deblending of the Herschel sources. Figure 1 shows thumbnails in several bands of two interesting sources detected by Herschel in the Bullet cluster field: the southern tip of the arc at z = 3.24 described in Mehlert et al (2001), and a sub-mm galaxy detected by LABOCA (source #10 in Johansson et al 2010). With these two examples, we demonstrate that the use of IRAC and MIPS data helps to correctly identify the Herschel sources with optical/NIR counterparts.…”

Section: Data and Catalogsmentioning

confidence: 87%

Improving the identification of high-zHerschelsources with position priors and optical/NIR and FIR/mm photometric redshifts

Pérez‐González

Egami

Rex

et al. 2010

A&A

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We present preliminary results about the detection of high redshift (U)LIRGs in the Bullet cluster field by the PACS and SPIRE instruments within the Herschel Lensing Survey (HLS) Program. We describe in detail a photometric procedure designed to recover robust fluxes and deblend faint Herschel sources near the confusion noise. The method is based on the use of the positions of Spitzer/MIPS 24 μm sources as priors. Our catalogs are able to reliably (5σ) recover galaxies with fluxes above 6 and 10 mJy in the PACS 100 and 160 μm channels, respectively, and 12 to 18 mJy in the SPIRE bands. We also obtain spectral energy distributions covering the optical through the far-infrared/millimeter spectral ranges of all the Herschel detected sources, and analyze them to obtain independent estimations of the photometric redshift based on either stellar population or dust emission models. We exemplify the potential of the combined use of Spitzer position priors plus independent optical and IR photometric redshifts to robustly assign optical/NIR counterparts to the sources detected by Herschel and other (sub-)mm instruments.

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Evidence for Chemical Evolution in Spectra of High Redshift Galaxies

Mehlert¹,

Noll²,

Appenzeller³

2003

The Evolution of Galaxies

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Using a sample of 57 VLT FORS spectra in the redshift range 1.37 < z < 3.40 (selected mainly from the FORS Deep Field survey) and a comparison sample with 36 IUE spectra of local (z ≈ 0) starburst galaxies we derive C iv and Si iv equivalent width values and estimate metallicities of starburst galaxies as a function of redshift. Assuming that a calibration of the C iv equivalent widths in terms of the metallicity based on the local sample of starburst galaxies is applicable to high-z objects, we find a significant increase of the average metallicities from about 0.16 Z at the cosmic epoch corresponding to z ≈ 3.2 to about 0.42 Z at z ≈ 2.3. A significant further increase in metallicity during later epochs cannot be detected in our data. Compared to the local starburst galaxies our high-redshift objects tend to be overluminous for a fixed metallicity. Our observational results are in good agreement with published observational data by other authors and with theoretical predictions of the cosmic chemical evolution.

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Gravitationally lensed high redshift galaxies in the field of 1E0657-56

Cited by 29 publications

References 27 publications

Galaxy Evolution Insights from Spectral Modeling of Large Data Sets from the Sloan Digital Sky Survey

Galaxy Evolution Insights from Spectral Modeling of Large Data Sets from the Sloan Digital Sky Survey

Improving the identification of high-zHerschelsources with position priors and optical/NIR and FIR/mm photometric redshifts

Evidence for Chemical Evolution in Spectra of High Redshift Galaxies

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