Curtis Schmidt-thin prism survey for extragalactic emission-line objects - University of Michigan List I

MacAlpine, G. M.; Smith, Scott; Lewis, David

doi:10.1086/190444

Cited by 75 publications

(32 citation statements)

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“…In order to study a sufficiently large SFDG sample for which comparable observational data are available, we decided to use lists IV and V of the sample of ELGs from the University of Michigan (UM) Survey (McAlpine et al 1977a(McAlpine et al , 1977b(McAlpine et al , 1977cMcAlpine & Lewis 1978;McAlpine & Williams 1981), systematically investigated in Salzer et al (1989aSalzer et al ( , 1989b by means of spectroscopy and CCD imaging in B and V . Among the different types of ELGs, all objects classified as H ii galaxies were selected; the magnitude limit of M B > −18 mag, commonly adopted to select dwarf galaxies, was applied after the distance correction (Sect.…”

Section: Sample Selectionmentioning

confidence: 99%

On faint companions in the close environment of star-forming dwarf galaxies

Noeske

Iglésias-Páramo

Vı́lchez

et al. 2001

A&A

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Abstract.We have searched for companion galaxies in the close environment of 98 star-forming dwarf galaxies (SFDGs) from field and low density environments, using the NASA Extragalactic Database. Most of the companions are dwarf galaxies which due to observational selection effects were previously disregarded in environmental studies of SFDGs. A subsample at low redshift, cz < 2000 km s −1 , was chosen to partially eliminate the observational bias against distant dwarf companions. We find companion candidates for approximately 30% of the objects within a projected linear separation sp < 100 kpc and a redshift difference ∆cz < 500 km s −1 . The limited completeness of the available data sets, together with the non-negligible frequency of H i clouds in the vicinity of SFDGs indicated by recent radio surveys, suggest that a considerably larger fraction of these galaxies may be accompanied by low-mass systems. This casts doubt on the hypothesis that the majority of them can be considered truly isolated. The velocity differences between companion candidates and sample SFDGs amount typically to < ∼ 250 km s −1 , and show a rising distribution towards lower ∆cz. This is similarly found for dwarf satellites of spiral galaxies, suggesting a physical association between the companion candidates and the sample SFDGs. SFDGs with a close companion do not show significant differences in their Hβ equivalent widths and B −V colours as compared to isolated ones. However, the available data do not allow us to rule out that interactions with close dwarf companions can influence the star formation activity in SFDGs.

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Section: Sample Selectionmentioning

confidence: 99%

On faint companions in the close environment of star-forming dwarf galaxies

Noeske

Iglésias-Páramo

Vı́lchez

et al. 2001

A&A

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“…These surveys focused primarily on UV/Optical (λ<0.5 μm) low-resolution spectroscopy of emission lines. Many surveys continued over the decades, e.g., Markarian (1967), Smith (1975), MacAlpine et al (1977), and Wasilewski (1983), helping to discover and catalog quasars and emission-line galaxies, as well as the search for young stars and their places of formation, within our own Galaxy, e.g., Dahm (2005). Grism surveys can be more efficient, requiring less observing time to reach a given S/N, than their slit/grating counterparts, and can be significantly more robust and reliable than photometric redshift surveys, e.g., Smith (1978) and Schmidt et al (1986).…”

Section: Introductionmentioning

confidence: 99%

FIGS—Faint Infrared Grism Survey: Description and Data Reduction

Pirzkal

Malhotra

Ryan

et al. 2017

ApJ

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The Faint Infrared Grism Survey (FIGS) is a deep Hubble Space Telescope (HST) WFC3/IR (Wide Field Camera 3 Infrared) slitless spectroscopic survey of four deep fields. Two fields are located in the Great Observatories Origins Deep Survey-North (GOODS-N) area and two fields are located in the Great Observatories Origins Deep Survey-South (GOODS-S) area. One of the southern fields selected is the Hubble Ultra Deep Field. Each of these four fields were observed using the WFC3/G102 grism (0.8 μm-1.15 μm continuous coverage) with a total exposure time of 40 orbits (≈100 kilo-seconds) per field. This reaches a s 3 continuum depth of »26 AB magnitudes and probes emission lines to~---10 erg s cm 17 12 . This paper details the four FIGS fields and the overall observational strategy of the project. A detailed description of the Simulation Based Extraction (SBE) method used to extract and combine over 10,000 spectra of over 2000 distinct sources brighter than = m 26.5mag is provided. High fidelity simulations of the observations is shown to significantly improve the background subtraction process, the spectral contamination estimates, and the final flux calibration. This allows for the combination of multiple spectra to produce a final high quality, deep, 1D spectra for each object in the survey.

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“…• wide strip of the University of Michigan (UM) Survey (MacAlpine et al 1977;Salzer et al 1989b and references therein) and of several fields of the Heidelberg void survey (HVS) (Hopp & Kuhn 1995;Popescu et al 1996) there are no large deep surveys in this region. It will be covered in the near future by two 1.5…”

Section: Introductionmentioning

confidence: 99%

The Hamburg/SAO Survey for low metallicity blue compact H II galaxies (HSS–LM)

Ugryumov

Engels

Pustilnik

et al. 2002

A&A

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Abstract. We present the description and the first results of a new project devoted to the search for extremely metaldeficient blue compact/H -galaxies (BCGs) and to the creation of a well selected large BCG sample with strong emission lines. Such galaxies should be suitable for reliable determination of their oxygen abundance through the measurement of the faint [O ] λ 4363 Å line. The goals of the project are two-fold: a) to discover a significant number of new extremely metalpoor galaxies (Z 1/20 Z ), and b) to study the metallicity distribution of local BCGs. Selection of candidates for follow-up slit spectroscopy is performed on the database of objective prism spectra of the Hamburg Quasar Survey. The sky region is limited by δ ≥ 0• and b II ≤ −30• . In this paper we present the results of the follow-up spectroscopy conducted with the Russian 6 m telescope. The list of observed candidates contained 52 objects, of which 46 were confirmed as strong-lined BCGs (EW([O ] λ 5007) ≥ 100 Å). The remaining five lower excitation ELGs include three BCGs, and two galaxies classified as SBN (Starburst Nucleus) and DANS (Dwarf Amorphous Nucleus Starburst). One object is identified as a quasar with a strong Lyα emission line near λ 5000 Å (z ∼ 3). We provide a list with coordinates, measured radial velocities, B-magnitudes, equivalent widths EW([O ] λ 5007) and EW(Hβ) and for the 46 strong-lined BCGs the derived oxygen abundances 12+log(O/H). The abundances range between 7.42 and 8.4 (corresponding to metallicities between 1/30 and 1/3 Z ). The sample contains four galaxies with Z 1/20 Z , of which three are new discoveries. This demonstrates the high efficiency of the new project to find extremely metal-deficient galaxies. The radial velocities of the strong-lined ELGs range between 500 and 19 000 km s −1 with a median value of ∼6400 km s −1 . The typical B-magnitudes of the galaxies presented are 17. m 0−18. m 0.

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Curtis Schmidt-thin prism survey for extragalactic emission-line objects - University of Michigan List I

Cited by 75 publications

References 0 publications

On faint companions in the close environment of star-forming dwarf galaxies

On faint companions in the close environment of star-forming dwarf galaxies

FIGS—Faint Infrared Grism Survey: Description and Data Reduction

The Hamburg/SAO Survey for low metallicity blue compact H II galaxies (HSS–LM)

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