Survey Of Emission-line Galaxies Research Articles

Prime Focus Spectrograph: A very wide-field, massively multiplexed, optical & near-infrared spectrograph for Subaru Telescope

AbstractThis short article is about Prime Focus Spectrograph (PFS), a very wide-field, massively-multiplexed, and optical & near-infrared (NIR) spectrograph as a next generation facility instrument on Subaru Telescope. More details and updates are available on the PFS official website (http://pfs.ipmu.jp), blog (http://pfs.ipmu.jp/blog/), and references therein.The project, instrument, & timelinePFS will position 2400 fibers to science targets or blank sky in the 1.3 degree field on the Subaru prime focus. These fibers will be quickly (~60sec) reconfigurable and feed the photons during exposures to the Spectrograph System (SpS). SpS consists of 4 modules each of which accommodate ~600 fibers and deliver spectral images ranging from 380nm to 1260nm simultaneously at one exposure via the 3 arms of blue, red, and NIR cameras. The instrument development has been undertaken by the international collaboration at the initiative of Kavli IPMU. The project is now going into the construction phase aiming at system integration and on-sky engineering observations in 2017-2018, and science operation in 2019.The survey design has also been under development envisioning a survey spanning ~300 nights over ~5 years in the framework of Subaru Strategic Program (SSP). The key science areas are: Cosmology, galaxy/AGN evolution, and Galactic Archaeology (GA) (Takada et al. 2014). The cosmology program will be to constrain the nature of dark energy via a survey of emission line galaxies over a comoving volume of 10 Gpc3 at z=0.8-2.4. In the galaxy/AGN program, the wide wavelength coverage of PFS as well as the large field of view will be exploited to characterize the galaxy populations and its clustering properties over a wide redshift range. A survey of color-selected galaxies/AGN at z = 1-2 will be conducted over 20 square degrees yielding a fair sample of galaxies with stellar masses down to ~1010M⊙. In the GA program, radial velocities and chemical abundances of stars in the Milky Way, dwarf spheroids, and M31 will be used to understand the past assembly histories of those galaxies and the structures of their dark matter halos. Spectra will be taken for 1 million stars as faint as V = 22 mag therefore out to large distances from the Sun.PFS will provide powerful spectroscopic capabilities even in the era of Euclid, LSST, WFIRST and TMT, and the effective synergies are expected for further unique science outputs.

GLACE survey: OSIRIS/GTC tuneable filter Hαimaging of the rich galaxy cluster ZwCl 0024.0+1652 atz = 0.395

The cores of clusters at 0 $\lesssim$ z $\lesssim$ 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type ones. Galaxy properties, notably the star formation (SF) ability, are altered as they fall into overdense regions. The critical issues to understand this evolution are how the truncation of SF is connected to the morphological transformation and the responsible physical mechanism. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a study on the variation of galaxy properties (SF, AGN, morphology) as a function of environment in a representative sample of clusters. A deep survey of emission line galaxies (ELG) is being performed, mapping a set of optical lines ([OII], [OIII], H$\beta$ and H$\alpha$/[NII]) in several clusters at z $\sim$ 0.40, 0.63 and 0.86. Using the Tunable Filters (TF) of OSIRIS/GTC, GLACE applies the technique of TF tomography: for each line, a set of images at different wavelengths are taken through the TF, to cover a rest frame velocity range of several thousands km/s. The first GLACE results target the H$\alpha$/[NII] lines in the cluster ZwCl 0024.0+1652 at z = 0.395 covering $\sim$ 2 $\times$ r$_{vir}$. We discuss the techniques devised to process the TF tomography observations to generate the catalogue of H$\alpha$ emitters of 174 unique cluster sources down to a SFR below 1 M$_{\odot}$/yr. The AGN population is discriminated using different diagnostics and found to be $\sim$ 37% of the ELG population. The median SFR is 1.4 M$_{\odot}$/yr. We have studied the spatial distribution of ELG, confirming the existence of two components in the redshift space. Finally, we have exploited the outstanding spectral resolution of the TF to estimate the cluster mass from ELG dynamics, finding M$_{200}$ = 4.1 $\times$ 10$^{14}$ M$_{\odot} h^{-1}$, in agreement with previous weak-lensing estimates.

Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph

Abstract The Subaru Prime Focus Spectrograph (PFS) is a massively multiplexed fiber-fed optical and near-infrared three-arm spectrograph (Nfiber = 2400, 380 ≤ λ ≤ 1260 nm, 1 $_{.}^{\circ}$3 diameter field of view). Here, we summarize the science cases in terms of provisional plans for a 300-night Subaru survey. We describe plans to constrain the nature of dark energy via a survey of emission line galaxies spanning a comoving volume of 9.3 h−3 Gpc3 in the redshift range 0.8 < z < 2.4. In each of six redshift bins, the cosmological distances will be measured to 3% precision via the baryonic acoustic oscillation scale, and redshift-space distortion measures will constrain structure growth to 6% precision. In the near-field cosmology program, radial velocities and chemical abundances of stars in the Milky Way and M 31 will be used to infer the past assembly histories of spiral galaxies and the structure of their dark matter halos. Data will be secured for 106 stars in the Galactic thick-disk, halo, and tidal streams as faint as V ∼ 22, including stars with V < 20 to complement the goals of the Gaia mission. A medium-resolution mode with R = 5000 to be implemented in the red arm will allow the measurement of multiple α-element abundances and more precise velocities for Galactic stars. For the galaxy evolution program, our simulations suggest the wide wavelength range of PFS will be powerful in probing the galaxy population and its clustering over a wide redshift range. We plan to conduct a color-selected survey of 1 < z < 2 galaxies and AGN over 16 deg2 to J ≃ 23.4, yielding a fair sample of galaxies with stellar masses above ∼1010 M⊙ at z ≃ 2. A two-tiered survey of higher redshift Lyman break galaxies and Lyman alpha emitters will quantify the properties of early systems close to the reionization epoch.

GRB 091127/SN 2009nz and the VLT/X-shooter spectroscopy of its host galaxy: probing the faint end of the mass-metallicity relation

We perform a detailed study of the gamma-ray burst GRB091127/SN2009nz host galaxy at z=0.490 using the VLT/X-shooter spectrograph in slit and integral-field unit (IFU). From the analysis of the optical and X-ray afterglow data obtained from ground-based telescopes and Swift-XRT we confirm the presence of a bump associated with SN2009nz and find evidence of a possible jet break in the afterglow lightcurve. The X-shooter afterglow spectra reveal several emission lines from the underlying host, from which we derive its integrated properties. These are in agreement with those of previously studied GRB-SN hosts and, more generally, with those of the long GRB host population. We use the Hubble Space Telescope and ground based images of the host to determine its stellar mass (M_star). Our results extend to lower M_star values the M-Z plot derived for the sample of long GRB hosts at 0.3<z<1.0 adding new information to probe the faint end of the M-Z relation and the shift of the LGRB host M-Z relation from that found from emission line galaxy surveys. Thanks to the IFU spectroscopy we can build the 2D velocity, velocity dispersion and star formation rate (SFR) maps. They show that the host galaxy has a perturbed rotation kinematics with evidence of a SFR enhancement consistent with the afterglow position.

Stellar Populations in Local Star‐forming Galaxies

The main goal of this thesis work is studying the main properties of the stellar populations embedded in a statistically complete sample of local active star-forming galaxies: the Universidad Complutense de Madrid (UCM) Survey of emission-line galaxies. This sample contains 191 local star-forming galaxies at an average redshift of 0.026. The survey was carried out using an objective-prism technique centered at the wavelength of the Halpha nebular emission-line (a common tracer of recent star formation). (continues)

Hamburg/SAO Survey of Emission-Line Galaxies

We present first results of the Hamburg/SAO Survey of emission-line galaxies (hereafter HSS, SAO—Special Astrophysical Observatory, Russia) initiated to search for extremely metal-deficient (Z&lt;Z⊙/10) galaxies and to create a large sample of Blue Compact Galaxies (BCG). This “Northern BCG Sample,” will be assembled by merging the HSS with samples from the Second Byurakan Survey (SBS) (Stepanianet al.1987) and the Case Low-Dispersion Northern Sky Survey (Peschet al.1991).

PHOTOMETRIC AND MORPHOLOGICAL ANALYSIS OF UCM GALAXIES

ABSTRACT A set of 212 objects of the UCM (Universidad Complutense de Madrid) survey of emission-line galaxies (ELGs), selected from objective prism plates by the presence of H-alpha emission in their spectra, has been analysed in the Thuan & Gunn r filter. From CCD images of these UCM objects we have obtained the fundamental photometric parameters (apparent and absolute magnitudes, linear diameters) and a set of characteristic morphological parameters extracted by surface photometry techniques (parameters of bulb + disk decomposition, concentration indexes and mean surface brightnesses). From this information, we have carried out intrinsecal statistical analysis of the data in the UCM sample and extrinsecal comparison with other samples of galaxies. And specially, we have simultaneously applied, for the first time in a sample of ELGs, five morphological criteria in order to obtain the Hubble type of these galaxies. As results of this work we have obtained that the UCM survey is specially effective in the detection of ELGs smaller and less luminous than normal spirals (the median values of the UCM sample are Mr = -20.6 and D24 = 19.4 kpc) and that emission arises fundamentally from the nuclear regions of the galaxies (only 22% of the sample show emitting knots outside the nucleus). Morphologically, the UCM sample is dominated by late-type galaxies, with 66% being Sb or later. This result confirms the expected tendency of the ELGs to be advanced type galaxies due to the higher mass fraction in gas available in these systems. Specially, we have found 9 candidates to BCD (blue compact dwarf galaxy), five of them previously unknown. We have also obtained that 10% of the UCM ELGs present typical parameters of S0 types, supporting the idea that not all S0 galaxies are dead systems without prominent recent star formation, and that in the subsample of 16 UCM galaxies showing obvious signs of interactions, 25% are S0 type galaxies. Finally, we have analysed the influence of the medium in the occurence and nature of the ELGs. So, we have compared the presence of ELGs and their morphologies in a subsample of galaxies in the Coma cluster respect to the subsample of field galaxies. Then, we have found that whereas 34% of the field Zwicky galaxies are ELGs, this fraction is reduced to 9% in the Coma cluster, consistent with the known efect that the fraction of galaxies that are ELGs is much lower in high-density cluster environments than in the field due to the lower fraction of star forming gas available in these dense media. And respect to the morphology, the objective prism technique permits to reveal, inside a cluster globally dominated by E-S0 type galaxies, a population of ELGs with 71% being Sb type or later. In the future, we propose to study in others filters the subset of these UCM galaxies specially peculiar, like the BCD galaxies (candidates to low metalicity objects), irregular and interacting systems, and to continue investigating the conexion between the medium and the presence of ELGs and its influence on the morphology of these galaxies.

Survey of emission-line galaxies: Universidad Complutense de Madrid list

view Abstract Citations (82) References (67) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Survey of Emission-Line Galaxies: Universidad Complutense de Madrid List 1 Zamorano, J. ; Rego, M. ; Gallego, J. G. ; Vitores, A. G. ; Gonzalez-Riestra, R. ; Rodriguez-Caderot, G. Abstract A low-dispersion objective-prism survey for low-redshift emission-line galaxies (ELGs) is being carried out by the University Complutense de Madrid with the Schmidt telescope at the German-Spanish Observatory of Calar Alto (Almeria, Spain). A 4^deg^ full aperture prism, which provides a dispersion of 1950 A mm^-1^, and IIIaF emulsion combination has been used to search for ELGs selected by the presence of Hα emission in their spectra. Our survey has proved to be able to recover objects already found by similar surveys with different techniques and, what is more important, to discover new objects not previously cataloged. A compilation of descriptions and positions, along with finding charts when necessary, is presented for 160 extragalactic emission-line objects. This is the first list, which contains objects located in a region of the sky covering 270 deg^2^ in 10 fields near α = 0^h^ and δ = 20^deg^. Publication: The Astrophysical Journal Supplement Series Pub Date: December 1994 DOI: 10.1086/192103 Bibcode: 1994ApJS...95..387Z Keywords: Astronomical Catalogs; Emission Spectra; H Alpha Line; Red Shift; Seyfert Galaxies; Sky Surveys (Astronomy); Astronomical Observatories; Astronomical Spectroscopy; Extraterrestrial Radiation; Schmidt Telescopes; Spain; Astronomy; GALAXIES: GENERAL; SURVEYS; GALAXIES: SEYFERT full text sources ADS | data products SIMBAD (160) NED (160) CDS (2) Related Materials (1) Catalog: 1997yCat..20950387Z

Slitless Spectroscopy by Photographic and CCD Detectors Across Large Fields

We present a new survey of emission line galaxies, performed with the ESO 1 m Schmidt telescope equipped with the 4° objective prism using IIIa-J photographic emulsion. The plates are digitized with the MAMA microdensitometer. A subsequent reduction of the block scans gives redshifts with a mean accuracy of 160 km/s−1, and spectrophotometric measurements of the intensity and equivalent widths of the principal emission lines. A brief discussion is given of the possible extension of quantitative reduction of slitless spectroscopy to archive plates and future large CCD array frames.

An Automatic Approach for Selecting New HA Emission-Line Galaxies

The most unambiguous way to discover new emission-line galaxies (ELGs) is directly by the presence of their lines, using objective-prism plates of adequate resolution. The first survey using this technique was developed by Smith in 1975 with the 0.6 m CTIO Curtis Schmidt Telescope. The Universidad Complutense de Madrid (UCM) is carrying out a survey of ELGs with the Schmidt Telescope at Calar Alto (Almería, Spain) using the presence of Ha in emission in IIIa-F prism plates as selection criterion. The observational procedure and results are described in Rego et al. 1989; Zamorano et al. 1990; Zamorano et al. 1993.

Objective prism survey of emission-line galaxies. IV

This is the fourth paper in the series giving the results of an objective prism survey of emission line galaxies using the Beijing Observatory 60 cm Schmidt. TABLE 1 contains 100 emission line objects, of which 96 are emission line galaxies, 3 are planetary nebulae and 1 is an emission line star. Of the emission line galaxies, 69 or 72% are of types s or sd; 27 or 28% are of types d and ds. In addition to 4 known Seyfert galaxies there are at least 5 probable Seyferts. 23 of the objects are IRAS sources, all being connected with strong emission phenomena.

An objective prism survey of emission line galaxies

An object prism survey of emission line galaxies was begun in 1981 at Beijing Observatory. This paper is the first one of the present survey, giving the first list of emission line objects detected. We used a 60 90 Schmidt telescope with a 5.3° objective prism and IIIa J emulsion, which proved to be an efficient instrument for isolating emission line galaxies. On a dozen plates covering some 220 square degrees of sky, 50 emission line objects were detected, 47 of which are galaxies and the other 3 are planetary nebulae. Their finding charts are given.