The MUSE Hubble Ultra Deep Field Survey

We present the MUSE Hubble Ultra Deep Survey, a mosaic of nine MUSE fields covering 90% of the entire HUDF region with a 10-h deep exposure time, plus a deeper 31-h exposure in a single 1.15 arcmin2 field. The improved observing strategy and advanced data reduction results in datacubes with sub-arcsecond spatial resolution (0.̋65 at 7000 Å) and accurate astrometry (0.̋07 rms). We compare the broadband photometric properties of the datacubes to HST photometry, finding a good agreement in zeropoint up to mAB = 28 but with an increasing scatter for faint objects. We have investigated the noise properties and developed an empirical way to account for the impact of the correlation introduced by the 3D drizzle interpolation. The achieved 3σ emission line detection limit for a point source is 1.5 and 3.1 × 10-19 erg s-1 cm-2 for the single ultra-deep datacube and the mosaic, respectively. We extracted 6288 sources using an optimal extraction scheme that takes the published HST source locations as prior. In parallel, we performed a blind search of emission line galaxies using an original method based on advanced test statistics and filter matching. The blind search results in 1251 emission line galaxy candidates in the mosaic and 306 in the ultradeep datacube, including 72 sources without HST counterparts (mAB > 31). In addition 88 sources missed in the HST catalog but with clear HST counterparts were identified. This data set is the deepest spectroscopic survey ever performed. In just over 100 h of integration time, it provides nearly an order of magnitude more spectroscopic redshifts compared to the data that has been accumulated on the UDF over the past decade. The depth and high quality of these datacubes enables new and detailed studies of the physical properties of the galaxy population and their environments over a large redshift range.

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Study of a Complete Sample of Hα Emission–Line Galaxies from the UCM Survey

Symposium - International Astronomical Union ◽

10.1017/s0074180900232993 ◽

1996 ◽

Vol 171 ◽

pp. 380-380 ◽

Cited By ~ 1

Author(s):

J. Gallego ◽

J. Zamorano ◽

M. Rego ◽

A.G. Vitores ◽

O. Alonso

Keyword(s):

Star Formation ◽

Emission Line ◽

Energy Output ◽

University Of Michigan ◽

Complete Sample ◽

Star Forming ◽

The Galaxy ◽

Hα Emission ◽

Emission Line Galaxies ◽

Galaxy Population

The Universidad Complutense de Madrid survey is a long-term project with the aim of finding and analyzing star forming galaxies using the Hα line as the tracer for star formation processes. In order to obtain a representative and complete sample of the population detected, spectroscopic observations were carried out for the full sample of Hα emission-line galaxy (ELG) candidates of the UCM lists 1 and 2. The ELGs types most commonly found (47%) are intermediate to low-luminosity objects with a very intense star-formation region which dominates the optical energy output of the galaxy. This kind of ELGs is similar to the galaxy population detected in the blue objective-prism surveys. And what is more important, a second population (43%) of star-forming galaxies with low ionization or high extinction properties has been found. This ELGs group is detected neither in the blue (University of Michigan survey, Case survey) nor in other surveys (Kiso, IRAS, Markarian) using other selection techniques.

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The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: exploring the halo occupation distribution model for emission line galaxies

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2951 ◽

2020 ◽

Vol 499 (4) ◽

pp. 5486-5507 ◽

Cited By ~ 4

Author(s):

S Avila ◽

V Gonzalez-Perez ◽

F G Mohammad ◽

A de Mattia ◽

C Zhao ◽

...

Keyword(s):

Emission Line ◽

Galaxy Formation ◽

Distribution Model ◽

Galaxy Formation And Evolution ◽

Formation And Evolution ◽

Physical Effects ◽

Emission Line Galaxies ◽

Halo Masses ◽

The Impact ◽

Halo Occupation Distribution

ABSTRACT We study the modelling of the halo occupation distribution (HOD) for the eBOSS DR16 emission line galaxies (ELGs). Motivated by previous theoretical and observational studies, we consider different physical effects that can change how ELGs populate haloes. We explore the shape of the average HOD, the fraction of satellite galaxies, their probability distribution function (PDF), and their density and velocity profiles. Our baseline HOD shape was fitted to a semi-analytical model of galaxy formation and evolution, with a decaying occupation of central ELGs at high halo masses. We consider Poisson and sub/super-Poissonian PDFs for satellite assignment. We model both Navarro–Frenk–White and particle profiles for satellite positions, also allowing for decreased concentrations. We model velocities with the virial theorem and particle velocity distributions. Additionally, we introduce a velocity bias and a net infall velocity. We study how these choices impact the clustering statistics while keeping the number density and bias fixed to that from eBOSS ELGs. The projected correlation function, wp, captures most of the effects from the PDF and satellites profile. The quadrupole, ξ2, captures most of the effects coming from the velocity profile. We find that the impact of the mean HOD shape is subdominant relative to the rest of choices. We fit the clustering of the eBOSS DR16 ELG data under different combinations of the above assumptions. The catalogues presented here have been analysed in companion papers, showing that eBOSS RSD+BAO measurements are insensitive to the details of galaxy physics considered here. These catalogues are made publicly available.

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A stellar census in globular clusters with MUSE: A spectral catalogue of emission-line sources

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936485 ◽

2019 ◽

Vol 631 ◽

pp. A118 ◽

Cited By ~ 7

Author(s):

Fabian Göttgens ◽

Tim-Oliver Husser ◽

Sebastian Kamann ◽

Stefan Dreizler ◽

Benjamin Giesers ◽

...

Keyword(s):

Emission Line ◽

Binary Stars ◽

Globular Clusters ◽

Cataclysmic Variables ◽

Variable Stars ◽

Emission Lines ◽

Data Set ◽

Stellar Spectra ◽

X Ray ◽

Emission Line Galaxies

Aims. Globular clusters produce many exotic stars due to a much higher frequency of dynamical interactions in their dense stellar environments. Some of these objects were observed together with several hundred thousand other stars in our MUSE survey of 26 Galactic globular clusters. Assuming that at least a few exotic stars have exotic spectra (i.e. spectra that contain emission lines), we can use this large spectroscopic data set of over a million stellar spectra as a blind survey to detect stellar exotica in globular clusters. Methods. To detect emission lines in each spectrum, we modelled the expected shape of an emission line as a Gaussian curve. This template was used for matched filtering on the differences between each observed 1D spectrum and its fitted spectral model. The spectra with the most significant detections of Hα emission are checked visually and cross-matched with published catalogues. Results. We find 156 stars with Hα emission, including several known cataclysmic variables (CV) and two new CVs, pulsating variable stars, eclipsing binary stars, the optical counterpart of a known black hole, several probable sub-subgiants and red stragglers, and 21 background emission-line galaxies. We find possible optical counterparts to 39 X-ray sources, as we detected Hα emission in several spectra of stars that are close to known positions of Chandra X-ray sources. This spectral catalogue can be used to supplement existing or future X-ray or radio observations with spectra of potential optical counterparts to classify the sources.

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The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the BAO and growth rate of structure of the emission line galaxy sample from the anisotropic power spectrum between redshift 0.6 and 1.1

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3891 ◽

2020 ◽

Author(s):

Arnaud de Mattia ◽

Vanina Ruhlmann-Kleider ◽

Anand Raichoor ◽

Ashley J Ross ◽

Amélie Tamone ◽

...

Keyword(s):

Growth Rate ◽

Power Spectrum ◽

Emission Line ◽

Large Scale ◽

Sloan Digital Sky Survey ◽

Full Data ◽

Data Set ◽

Weak Preference ◽

Galaxy Sample ◽

Emission Line Galaxies

Abstract We analyse the large-scale clustering in Fourier space of emission line galaxies (ELG) from the Data Release 16 of the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey. The ELG sample contains 173,736 galaxies covering 1,170 square degrees in the redshift range 0.6 < z < 1.1. We perform a BAO measurement from the post-reconstruction power spectrum monopole, and study redshift space distortions (RSD) in the first three even multipoles. Photometric variations yield fluctuations of both the angular and radial survey selection functions. Those are directly inferred from data, imposing integral constraints which we model consistently. The full data set has only a weak preference for a BAO feature (1.4σ). At the effective redshift zeff = 0.845 we measure $D_{\rm V}(z_{\rm eff})/r_{\rm drag} = 18.33_{-0.62}^{+0.57}$, with DV the volume-averaged distance and rdrag the comoving sound horizon at the drag epoch. In combination with the RSD measurement, at zeff = 0.85 we find $f\sigma _8(z_{\rm eff}) = 0.289_{-0.096}^{+0.085}$, with f the growth rate of structure and σ8 the normalisation of the linear power spectrum, $D_{\rm H}(z_{\rm eff})/r_{\rm drag} = 20.0_{-2.2}^{+2.4}$ and DM(zeff)/rdrag = 19.17 ± 0.99 with DH and DM the Hubble and comoving angular distances, respectively. These results are in agreement with those obtained in configuration space, thus allowing a consensus measurement of fσ8(zeff) = 0.315 ± 0.095, $D_{\rm H}(z_{\rm eff})/r_{\rm drag} = 19.6_{-2.1}^{+2.2}$ and DM(zeff)/rdrag = 19.5 ± 1.0. This measurement is consistent with a flat ΛCDM model with Planck parameters.

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Morphology and Evolution of Emission‐Line Galaxies in the Hubble Ultra Deep Field

The Astrophysical Journal ◽

10.1086/498129 ◽

2006 ◽

Vol 636 (2) ◽

pp. 582-591 ◽

Cited By ~ 13

Author(s):

N. Pirzkal ◽

C. Xu ◽

I. Ferreras ◽

S. Malhotra ◽

B. Mobasher ◽

...

Keyword(s):

Emission Line ◽

Emission Line Galaxies ◽

Hubble Ultra Deep Field

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J-PLUS: Synthetic galaxy catalogues with emission lines for photometric surveys

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936232 ◽

2019 ◽

Vol 631 ◽

pp. A82 ◽

Cited By ~ 3

Author(s):

David Izquierdo-Villalba ◽

Raul E. Angulo ◽

Alvaro Orsi ◽

Guillaume Hurier ◽

Gonzalo Vilella-Rojo ◽

...

Keyword(s):

Emission Line ◽

Narrow Band ◽

Spectral Energy Distribution ◽

Broad Band ◽

Line Emission ◽

Spectral Energy ◽

Filter Method ◽

Medium Band ◽

Emission Line Galaxies ◽

The Impact

We present a synthetic galaxy lightcone specially designed for narrow-band optical photometric surveys. To reduce time-discreteness effects, unlike previous works, we directly include the lightcone construction in the L-Galaxies semi-analytic model applied to the subhalo merger trees of the Millennium simulation. Additionally, we add a model for the nebular emission in star-forming regions, which is crucial for correctly predicting the narrow- and medium-band photometry of galaxies. Specifically, we consider, individually for each galaxy, the contribution of 9 different lines: Lyα (1216 Å), Hβ (4861 Å), Hα (6563 Å), [O II] (3727 Å, 3729 Å), [O III] (4959 Å, 5007 Å), [Ne III] (3870 Å), [O I] (6300 Å), [N II] (6548 Å, 6583 Å), and [S II] (6717 Å, 6731 Å). We validate our lightcone by comparing galaxy number counts, angular clustering, and Hα, Hβ, [O II], and [O III]5007 luminosity functions to a compilation of observations. As an application of our mock lightcones, we generated catalogues tailored for J-PLUS, a large optical galaxy survey featuring five broad-band and seven medium-band filters. We study the ability of the survey to correctly identify, with a simple three-filter method, a population of emission-line galaxies at various redshifts. We show that the 4000 Å break in the spectral energy distribution of galaxies can be misidentified as line emission. However, all significant excess (> 0.4 mag) can be correctly and unambiguously attributed to emission-line galaxies. Our catalogues are publicly released to facilitate their use in interpreting narrow-band surveys and in quantifying the impact of line emission in broad-band photometry.

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EMISSION-LINE GALAXIES FROM THE PEARS HUBBLE ULTRA DEEP FIELD: A 2D DETECTION METHOD AND FIRST RESULTS

The Astronomical Journal ◽

10.1088/0004-6256/135/4/1624 ◽

2008 ◽

Vol 135 (4) ◽

pp. 1624-1635 ◽

Cited By ~ 29

Author(s):

Amber N. Straughn ◽

Gerhardt R. Meurer ◽

Norbert Pirzkal ◽

Seth H. Cohen ◽

Sangeeta Malhotra ◽

...

Keyword(s):

Emission Line ◽

Detection Method ◽

First Results ◽

Emission Line Galaxies ◽

Hubble Ultra Deep Field

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The atomic gas of star-forming galaxies at z ∼ 0.05 as revealed by the Five-hundred-meter Aperture Spherical Radio Telescope

Astronomy and Astrophysics ◽

10.1051/0004-6361/202038483 ◽

2020 ◽

Vol 638 ◽

pp. L14 ◽

Cited By ~ 1

Author(s):

Cheng Cheng ◽

Edo Ibar ◽

Wei Du ◽

Juan Molina ◽

Gustavo Orellana-Gonzáles ◽

...

Keyword(s):

Emission Line ◽

Radio Telescope ◽

Line Emission ◽

Gas Content ◽

Dark Matter Halo ◽

Integration Time ◽

Dynamical Mass ◽

Star Forming ◽

Order Of Magnitude ◽

Atomic Gas

Context. We report new H I observations of four z ∼ 0.05 VALES galaxies undertaken during the commissioning phase of the Five-hundred-meter Aperture Spherical Radio Telescope (FAST). Aims. FAST is the largest single-dish telescope in the world, with a 500 m aperture and a 19-Beam receiver. Exploiting the unprecedented sensitivity provided by FAST, we aim to study the atomic gas content, via the H I 21 cm emission line, in low-z star formation galaxies taken from the Valparaíso ALMA/APEX Line Emission Survey (VALES). Together with previous Atacama Large Millimeter/submillimeter Array (ALMA) CO(J = 1−0) observations, the H I data provides crucial information to measure the gas mass and dynamics. Methods. As a pilot H I galaxy survey, we targeted four local star-forming galaxies at z ∼ 0.05. In particular, one of them has already been detected in H I by the Arecibo Legacy Fast ALFA survey (ALFALFA), allowing a careful comparison. We use an ON-OFF observing approach that allowed us to reach an rms of 0.7 mJy beam−1 at a 1.7 km s−1 velocity resolution within only 20 min ON-target integration time. Results. In this Letter, we demonstrate the extraordinary capability of the FAST 19-beam receiver to push the detectability of the H I emission line of extra-galactic sources. The H I emission line detected by FAST shows good consistency with the previous Arecibo telescope ALFALFA results. Our observations are put into context with previous multi-wavelength data to reveal the physical properties of these low-z galaxies. We find that the CO(J = 1−0) and H I emission line profiles are similar. The dynamical mass estimated from the H I data is an order of magnitude higher than the baryon mass and the dynamical mass derived from the CO observations, implying that the mass probed by dynamics of H I is dominated by the dark matter halo. In one case, a target shows an excess of CO(J = 1−0) in the line centre, which can be explained by an enhanced CO(J = 1−0) emission induced by a nuclear starburst showing high-velocity dispersion.

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The MUSE Hubble Ultra Deep Field Survey

Astronomy and Astrophysics ◽

10.1051/0004-6361/201731195 ◽

2017 ◽

Vol 608 ◽

pp. A2 ◽

Cited By ~ 66

Author(s):

H. Inami ◽

R. Bacon ◽

J. Brinchmann ◽

J. Richard ◽

T. Contini ◽

...

Keyword(s):

High Sensitivity ◽

Large Field ◽

Success Rates ◽

Redshift Distribution ◽

Color Selection ◽

Order Of Magnitude ◽

Deep Fields ◽

Hubble Ultra Deep Field ◽

Blind Search ◽

Magnitude Improvement

We have conducted a two-layered spectroscopic survey (1′ × 1′ ultra deep and 3′ × 3′ deep regions) in the Hubble Ultra Deep Field (HUDF) with the Multi Unit Spectroscopic Explorer (MUSE). The combination of a large field of view, high sensitivity, and wide wavelength coverage provides an order of magnitude improvement in spectroscopically confirmed redshifts in the HUDF; i.e., 1206 secure spectroscopic redshifts for Hubble Space Telescope (HST) continuum selected objects, which corresponds to 15% of the total (7904). The redshift distribution extends well beyond z> 3 and to HST/F775W magnitudes as faint as ≈ 30 mag (AB, 1σ). In addition, 132 secure redshifts were obtained for sources with no HST counterparts that were discovered in the MUSE data cubes by a blind search for emission-line features. In total, we present 1338 high quality redshifts, which is a factor of eight increase compared with the previously known spectroscopic redshifts in the same field. We assessed redshifts mainly with the spectral features [O ii] at z< 1.5 (473 objects) and Lyα at 2.9 <z< 6.7 (692 objects). With respect to F775W magnitude, a 50% completeness is reached at 26.5 mag for ultra deep and 25.5 mag for deep fields, and the completeness remains ≳ 20% up to 28–29 mag and ≈ 27 mag, respectively. We used the determined redshifts to test continuum color selection (dropout) diagrams of high-z galaxies. The selection condition for F336W dropouts successfully captures ≈ 80% of the targeted z ~ 2.7 galaxies. However, for higher redshift selections (F435W, F606W, and F775W dropouts), the success rates decrease to ≈ 20–40%. We empirically redefine the selection boundaries to make an attempt to improve them to ≈ 60%. The revised boundaries allow bluer colors that capture Lyα emitters with high Lyα equivalent widths falling in the broadbands used for the color-color selection. Along with this paper, we release the redshift and line flux catalog.

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Age at Exposure to Parental Suicide and the Subsequent Risk of Suicide in Young People

Crisis ◽

10.1027/0227-5910/a000468 ◽

2018 ◽

Vol 39 (1) ◽

pp. 27-36 ◽

Cited By ~ 5

Author(s):

Kuan-Ying Lee ◽

Chung-Yi Li ◽

Kun-Chia Chang ◽

Tsung-Hsueh Lu ◽

Ying-Yeh Chen

Keyword(s):

Young People ◽

Proportional Hazards ◽

Proportional Hazards Model ◽

Cox Proportional Hazards ◽

Cox Proportional Hazards Model ◽

Birth Registry ◽

Data Set ◽

Parental Suicide ◽

The Impact ◽

Age At Exposure

Abstract. Background: We investigated the age at exposure to parental suicide and the risk of subsequent suicide completion in young people. The impact of parental and offspring sex was also examined. Method: Using a cohort study design, we linked Taiwan's Birth Registry (1978–1997) with Taiwan's Death Registry (1985–2009) and identified 40,249 children who had experienced maternal suicide (n = 14,431), paternal suicide (n = 26,887), or the suicide of both parents (n = 281). Each exposed child was matched to 10 children of the same sex and birth year whose parents were still alive. This yielded a total of 398,081 children for our non-exposed cohort. A Cox proportional hazards model was used to compare the suicide risk of the exposed and non-exposed groups. Results: Compared with the non-exposed group, offspring who were exposed to parental suicide were 3.91 times (95% confidence interval [CI] = 3.10–4.92 more likely to die by suicide after adjusting for baseline characteristics. The risk of suicide seemed to be lower in older male offspring (HR = 3.94, 95% CI = 2.57–6.06), but higher in older female offspring (HR = 5.30, 95% CI = 3.05–9.22). Stratified analyses based on parental sex revealed similar patterns as the combined analysis. Limitations: As only register-based data were used, we were not able to explore the impact of variables not contained in the data set, such as the role of mental illness. Conclusion: Our findings suggest a prominent elevation in the risk of suicide among offspring who lost their parents to suicide. The risk elevation differed according to the sex of the afflicted offspring as well as to their age at exposure.

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