Author: "Almaini, O" / Topic: surveys - Searchworks@Jio Institute Digital Library Search Results

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1. Increasing AGN sample completeness using long-term near-infrared variability.

Author: Green, K, Elmer, E, Maltby, D T, Almaini, O, Merrifield, M, and Hartley, W G
Subjects: ACTIVE galactic nuclei, ACTIVE galaxies, STELLAR activity, X-ray detection, STELLAR mass
Abstract: In this work, we use 8 years of deep near-infrared imaging to select and study a new set of 601 active galaxies identified through long-term near-infrared (NIR) variability in the UKIDSS Ultra Deep Survey (UDS). These objects are compared to 710 X-ray bright Active Galactic Nuclei (AGN) detected by the Chandra X-ray observatory. We show that infrared variability and X-ray emission select distinct sets of active galaxies, finding only a 37 per cent overlap of galaxies detected by both techniques and confirming NIR-variable AGN to be typically X-ray quiet. Examining the mass functions of the active galaxies shows that NIR variability detects AGN activity in galaxies over a significantly wider range of host stellar mass compared to X-ray detection. For example, at z ∼ 1, variable AGN are identified among approximately 1 per cent of galaxies in a roughly flat distribution above the stellar mass completeness limit (⁠|$\gt 10^{9}\rm \, {\rm M}_{\odot }$|⁠), while X-ray detection primarily identifies AGN in galaxies of higher mass (⁠|$\gt 10^{10}\rm \, {\rm M}_{\odot }$|⁠). We conclude that long-term near-infrared variability provides an important new tool for obtaining more complete samples of AGN in deep survey fields. [ABSTRACT FROM AUTHOR]
Published: 2024
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2. STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS

Author: Santini, P, Ferguson, HC, Fontana, A, Mobasher, B, Barro, G, Castellano, M, Finkelstein, SL, Grazian, A, Hsu, LT, Lee, B, Lee, S-K, Pforr, J, Salvato, M, Wiklind, T, Wuyts, S, Almaini, O, Cooper, MC, Galametz, A, Weiner, B, Amorin, R, Boutsia, K, Conselice, CJ, Dahlen, T, Dickinson, ME, Giavalisco, M, Grogin, NA, Guo, Y, Hathi, NP, Kocevski, D, Koekemoer, AM, Kurczynski, P, Merlin, E, Mortlock, A, Newman, JA, Paris, D, Pentericci, L, Simons, R, and Willner, SP
Subjects: Space Sciences, Physical Sciences, catalogs, galaxies: fundamental parameters, galaxies: high-redshift, galaxies: stellar content, surveys, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We present the public release of the stellar mass catalogs for the GOODS-S and UDS fields obtained using some of the deepest near-IR images available, achieved as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey project. We combine the effort from 10 different teams, who computed the stellar masses using the same photometry and the same redshifts. Each team adopted their preferred fitting code, assumptions, priors, and parameter grid. The combination of results using the same underlying stellar isochrones reduces the systematics associated with the fitting code and other choices. Thanks to the availability of different estimates, we can test the effect of some specific parameters and assumptions on the stellar mass estimate. The choice of the stellar isochrone library turns out to have the largest effect on the galaxy stellar mass estimates, resulting in the largest distributions around the median value (with a semi interquartile range larger than 0.1 dex). On the other hand, for most galaxies, the stellar mass estimates are relatively insensitive to the different parameterizations of the star formation history. The inclusion of nebular emission in the model spectra does not have a significant impact for the majority of galaxies (less than a factor of 2 for 80% of the sample). Nevertheless, the stellar mass for the subsample of young galaxies (age
Published: 2015

3. The VANDELS ESO public spectroscopic survey

Author: Garilli, B., Mclure, R., Pentericci, L., Franzetti, P., Gargiulo, A., Carnall, A., Cucciati, O., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., Dunlop, J., Elbaz, D., Finkelstein, S., Fontana, A., Fontanot, F., Fumana, M., Guaita, L., Hartley, W., Jarvis, M., Juneau, S., Maccagni, D., Mcleod, D., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Talia, M., Calabrò, A., Cresci, G., Fynbo, J., Hathi, N., Hibon, P., Koekemoer, A., Magliocchetti, M., Salvato, M., Vietri, G., Zamorani, G., Almaini, O., Balestra, I., Bardelli, S., Begley, R., Brammer, G., Bell, E., Bowler, R., Brusa, M., Buitrago, F., Caputi, C., Cassata, P., Charlot, S., Citro, A., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G., Ferguson, H., Fiore, F., Franco, M., Georgakakis, A., Giavalisco, M., Grazian, A., Hamadouche, M., Jung, I., Kim, S., Khusanova, Y., Le Fèvre, O., Longhetti, M., Lotz, J., Mannucci, F., Maltby, D., Matsuoka, K., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Roberts-Borsani, G., Rosario, D., Saldana-Lopez, A., Santini, P., Saxena, A., Schaerer, D., Schreiber, C., Stark, D., Tasca, L., Thomas, R., Vanzella, E., Wild, V., Williams, C., Zucca, E., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], surveys, cosmology: observations, galaxies: fundamental parameters, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: statistics, catalogs, Astrophysics::Galaxy Astrophysics
Abstract: International audience; VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high-signal-to-noise ratio, medium-resolution spectra of galaxies at redshifts between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We provide a detailed description of sample selection, observations, and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at i AB = 25. The high signal-to-noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5 Å allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-infrared photometry and physical parameters derived through fitting the spectral energy distribution. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range of 8.3 < Log( M * / M ⊙ ) < 11.7.
Published: 2021

4. Infrared lags in the light curves of AGNs measured using a deep survey.

Author: Elmer, E, Merrifield, M, Almaini, O, Hartley, W G, and Maltby, D T
Subjects: LIGHT curves, ACTIVE galactic nuclei, ACTIVE galaxies, SEYFERT galaxies
Abstract: Information on the structure around active galactic nuclei (AGNs) has long been derived from measuring lags in their varying light output at different wavelengths. In principle, infrared data would reach to larger radii, potentially even probing reprocessed radiation in any surrounding dusty torus. In practice, this has proved challenging because high quality data are required to detect such variability, and the observations must stretch over a long period to probe the likely month-scale lags in variability. In addition, large numbers of sources would need to be observed to start searching for any patterns in such lags. Here, we show that the UKIDSS Ultra Deep Survey, built up from repeated observations over almost a decade, provides an ideal data set for such a study. For 94 sources identified as strongly varying AGNs within its square-degree field, we find that the K -band light curves systematically lag the J -band light curves by an average of around a month. The lags become smaller at higher redshift, consistent with the band shift to optical rest-frame emission. The less luminous AGNs also display shorter lags, as would be expected if their physical size scales with luminosity. [ABSTRACT FROM AUTHOR]
Published: 2021
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5. The VANDELS ESO spectroscopic survey

Author: McLure, R. J., Pentericci, L., Cimatti, A., Dunlop, J. S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S. L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W. G., Iovino, A., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Mármol-Queraltó, E., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., and University of St Andrews. School of Physics and Astronomy
Subjects: high-redshift [Galaxies], QC Physics, NDAS, Astrophysics::Solar and Stellar Astrophysics, QB Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, evolution [Galaxies], star formation [Galaxies], Astrophysics::Galaxy Astrophysics, QC, QB
Abstract: VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO’s Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < λ < 1.0 μm) spectroscopy of ≃2100 galaxies within the redshift interval 1.0 ≤ z ≤ 7.0, over a total area of ≃ 0.2 deg2 centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z ≥ 3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < tint < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 ≤ z ≤ 5.5, b) massive quiescent galaxies at 1.0 ≤ z ≤ 2.5, c) fainter star-forming galaxies at 3.0 ≤ z ≤ 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection. Postprint
Published: 2018

6. The SCUBA-2 Cosmology Legacy Survey: 850 ?m maps, catalogues and number counts

Author: Geach, J. E., Dunlop, J. S., Halpern, M., Smail, Ian, van der Werf, P., Alexander, D. M., Almaini, O., Aretxaga, I., Arumugam, V., Asboth, V., Banerji, M., Beanlands, J., Best, P. N., Blain, A. W., Birkinshaw, M., Chapin, E. L., Chapman, S. C., Chen, C-C., Chrysostomou, A., Clarke, C., Clements, D. L., Conselice, C., Coppin, K. E. K., Cowley, W. I., Danielson, A. L. R., Eales, S., Edge, A. C., Farrah, D., Gibb, A., Harrison, C. M., Hine, N. K., Hughes, D., Ivison, R. J., Jarvis, M., Jenness, T., Jones, S. F., Karim, A., Koprowski, M., Knudsen, K. K., Lacey, C. G., Mackenzie, T., Marsden, G., McAlpine, K., McMahon, R., Meijerink, R., Micha?owski, M. J., Oliver, S. J., Page, M. J., Peacock, J. A., Rigopoulou, D., Robson, E. I., Roseboom, I., Rotermund, K., Scott, Douglas, Sarjeant, S., Simpson, C., Simpson, J. M., Smith, D. J. B., Spaans, M., Stanley, F., Stevens, J. A., Swinbank, A. M., Targett, T., Thomson, A. P., Valiante, E., Wake, D. A., Webb, T. M. A., Willott, C., Zavala, J. A., Zemcov, M., and Serjeant, S.
Subjects: surveys, galaxies: high-redshift, galaxies: evolution, cosmology: observations, catalogues
Abstract: We present a catalogue of ∼3000 submillimetre sources detected (≥3.5σ) at 850 μm over ∼5 deg2 surveyed as part of the James Clerk Maxwell Telescope (JCMT) SCUBA-2 Cosmology Legacy Survey (S2CLS). This is the largest survey of its kind at 850 μm, increasing the sample size of 850 μm selected submillimetre galaxies by an order of magnitude. The wide 850 μm survey component of S2CLS covers the extragalactic fields: UKIDSS-UDS, COSMOS, Akari-NEP, Extended Groth Strip, Lockman Hole North, SSA22 and GOODS-North. The average 1σ depth of S2CLS is 1.2 mJy beam−1, approaching the SCUBA-2 850 μm confusion limit, which we determine to be σc ≈ 0.8 mJy beam−1.We measure the 850 μm number counts, reducing the Poisson errors on the differential counts to approximately 4 per cent at S850 ≈ 3 mJy. With several independent fields, we investigate field-to-field variance, finding that the number counts on 0.5◦–1◦ scales are generally within 50 per cent of the S2CLS mean for S850 > 3 mJy, with scatter consistent with the Poisson and estimated cosmic variance uncertainties, although there is a marginal (2σ) density enhancement in GOODS-North. The observed counts are in reasonable agreement with recent phenomenological and semi-analytic models, although determining the shape of the faint-end slope (S850 < 3 mJy) remains a key test. The large solid angle of S2CLS allows us to measure the bright-end counts: at S850 >10 mJy there are approximately 10 sources per square degree, and we detect the distinctive up-turn in the number counts indicative of the detection of local sources of 850 μm emission, and strongly lensed high-redshift galaxies. All calibrated maps and the catalogue are made publicly available.
Published: 2017

7. Long-term NIR variability in the UKIDSS Ultra Deep Survey: a new probe of AGN activity at high redshift.

Author: Elmer, E, Almaini, O, Merrifield, M, Hartley, W G, Maltby, D T, Lawrence, A, Botti, I, and Hirst, P
Subjects: *ACTIVE galactic nuclei, *SEYFERT galaxies, *REDSHIFT, *X-ray imaging, *LIGHT curves, *STELLAR mass
Abstract: We present the first attempt to select active galactic nuclei (AGN) using long-term near-infrared (NIR) variability. By analysing the K -band light curves of all the galaxies in the UKIRT Infrared Deep Sky Survey (UKIDSS) Ultra Deep Survey, the deepest NIR survey over ∼1 deg2, we have isolated 393 variable AGN candidates. A comparison to other selection techniques shows that only half of the variable sources are also selected using either deep Chandra X-ray imaging or Infrared Array Camera (IRAC) colour selection, suggesting that using NIR variability can locate AGN that are missed by more standard selection techniques. In particular, we find that long-term NIR variability identifies AGN at low luminosities and in host galaxies with low stellar masses, many of which appear relatively X-ray quiet. [ABSTRACT FROM AUTHOR]
Published: 2020
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8. The UKIRT Infrared Deep Sky Survey Early Data Release

Author: Emerson, J., Davies, J., Dalton, G., Collins, R., Casali, M., Bryant, J., Van Breukelen, C., Lucas, P., Jameson, R., Hirst, P., Edge, A., Almaini, O., Adamson, A., Lawrence, A., Irwin, M., Hodgkin, S., Cross, N., Hambly, N., Warren, S., Dye, S., Co-Authors., 32, Rawlings, M., Pinfield, D., Nakajima, Y., Mortlock, D., Mcmahon, R., Mann, R., Lewis, J., Loveday, J., Lodieu, N., Leggett, S., Kerr, T., Kendall, T., Hewett, P., Gonzales-Solares, E., Foucaud, S., Evans, D., Davis, C., Weatherley, S., Walton, N., Varricatt, W., Sutorius, E., Smith, A., Sekiguchi, K., Riello, M., and Read, M.
Subjects: media_common.quotation_subject, Infrared telescope, FOS: Physical sciences, Astronomy & Astrophysics, Astrophysics, infrared : general, surveys, Observatory, astro-ph, 0201 Astronomical and Space Sciences, media_common, Remote sensing, Physics, CALIBRATION, COUNTS, Science & Technology, Astrophysics (astro-ph), Astronomy, Astronomy and Astrophysics, Small sample, 2MASS, Data set, Space and Planetary Science, Sky, Physical Sciences, Survey data collection, Data release, Data reduction
Abstract: This paper defines the UKIRT Infrared Deep Sky Survey (UKIDSS) Early Data Release (EDR). UKIDSS is a set of five large near-infra-red surveys defined by Lawrence et al. (2006), being undertaken with the UK Infra-red Telescope (UKIRT) Wide Field Camera (WFCAM). The programme began in May 2005 and has an expected duration of seven years. Each survey uses some or all of the broadband filter complement ZYJHK. The EDR is the first public release of data to the European Southern Observatory (ESO) community. All worldwide releases occur after a delay of 18 months from the ESO release. The EDR provides a small sample dataset, ~50 sq.deg (about 1% of the whole of UKIDSS), that is a lower limit to the expected quality of future survey data releases. In addition, an EDR+ dataset contains all EDR data plus extra data of similar quality, but for areas not observed in all of the required filters (amounting to ~220 sq.deg). The first large data release, DR1, will occur in mid-2006. We provide details of the observational implementation, the data reduction, the astrometric and photometric calibration, and the quality control procedures. We summarise the data coverage and quality (seeing, ellipticity, photometricity, depth) for each survey and give a brief guide to accessing the images and catalogues from the WFCAM Science Archive., Accepted by MNRAS. 30 pages, 15 figures (some at reduced resolution due to upload restrictions - full res version at http://surveys.roe.ac.uk/wsa/pubs.html)
Published: 2016

9. The SCUBA-2 Cosmology Legacy Survey: 850 µm maps, catalogues and number counts.

Author: Geach, J. E., Dunlop, J. S., Halpern, M., Smail, Ian, van der Werf, P., Alexander, D. M., Almaini, O., Aretxaga, I., Arumugam, V., Asboth, V., Banerji, M., Beanlands, J., Best, P. N., Blain, A. W., Birkinshaw, M., Chapin, E. L., Chapman, S. C., Chen, C-C., Chrysostomou, A., and Clarke, C.
Subjects: SUBMILLIMETER astronomy, TELESCOPES, GALACTIC redshift, PHENOMENOLOGICAL theory (Physics), GALACTIC evolution, METAPHYSICAL cosmology
Abstract: We present a catalogue of ~3000 submillimetre sources detected (=3.5s) at 850 µm over ~5 deg² surveyed as part of the James Clerk Maxwell Telescope (JCMT) SCUBA-2 Cosmology Legacy Survey (S2CLS). This is the largest survey of its kind at 850 µm, increasing the sample size of 850 µm selected submillimetre galaxies by an order of magnitude. The wide 850 µm survey component of S2CLS covers the extragalactic fields: UKIDSS-UDS, COSMOS, Akari-NEP, Extended Groth Strip, Lockman Hole North, SSA22 and GOODS-North. The average 1s depth of S2CLS is 1.2 mJy beam-1, approaching the SCUBA-2 850 µm confusion limit, which we determine to be sc ≈ 0.8 mJy beam-1.We measure the 850 µm number counts, reducing the Poisson errors on the differential counts to approximately 4 per cent at S850 ≈ 3 mJy. With several independent fields, we investigate field-to-field variance, finding that the number counts on 0.5°-1° scales are generally within 50 per cent of the S2CLS mean for S850 > 3 mJy, with scatter consistent with the Poisson and estimated cosmic variance uncertainties, although there is a marginal (2s) density enhancement in GOODS-North. The observed counts are in reasonable agreement with recent phenomenological and semi-analytic models, although determining the shape of the faint-end slope (S850 < 3 mJy) remains a key test. The large solid angle of S2CLS allows us to measure the bright-end counts: at S850 > 10 mJy there are approximately 10 sources per square degree, and we detect the distinctive up-turn in the number counts indicative of the detection of local sources of 850 µm emission, and strongly lensed high-redshift galaxies. All calibrated maps and the catalogue are made publicly available. [ABSTRACT FROM AUTHOR]
Published: 2017
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10. VizieR Online Data Catalog: ELAIS: final band-merged catalogue (Rowan-Robinson+, 2004)

Author: Rowan-Robinson, M., Lari, C., Perez-Fournon, I., Gonzalez-Solares, E. A., La Franca, F., Vaccari, M., Oliver, S., Carlotta Gruppioni, Ciliegi, P., Heraudeau, P., Serjeant, S., Efstathiou, A., Babbedge, T., Matute, I., Pozzi, F., Franceschini, A., Vaisanen, P., Afonso-Luis, A., Alexander, D. M., Almaini, O., Baker, A. C., Basilakos, S., Barden, M., Del Burgo, C., Bellas-Velidis, I., Cabrera-Guerra, F., Carballo, R., Cesarsky, C. J., Clements, D. L., Crockett, H., Danese, L., Dapergolas, A., Drolias, B., Eaton, N., Egami, E., Elbaz, D., Fadda, D., Fox, M., Genzel, R., Goldschmidt, P., Gonzalez-Serrano, J. I., Graham, M., Granato, G. L., Hatziminaoglou, E., Herbstmeier, U., Joshi, M., Kontizas, E., Kontizas, M., Kotilainen, J. K., Kunze, D., Lawrence, A., Lemke, D., Linden-Vornle, M. J. D., Mann, R. G., Marquez, I., Masegosa, J., Mcmahon, R. G., Miley, G., Missoulis, V., Mobasher, B., Morel, T., Norgaard-Nielsen, H., Omont, A., Papadopoulos, P., Puget, J. -L, Rigopoulou, D., Rocca-Volmerange, B., Sedgwick, N., Silva, L., Sumner, T., Surace, C., Vila-Vilaro, B., Werf, P., Verma, A., Vigroux, L., Villar-Martin, M., Willott, C. J., Carraminana, A., Mujica, R., Imperial College London, Instituto de Astrofisica de Canarias (IAC), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, AUTRES, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Laboratoire de Physico-Chimie des Polymères et des Milieux Dispersés (PPMD), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Space Telescope Science Institute (STSci), Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Fisica de Plasmas (GoLP), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Oxford Astrophysics, Università degli Studi di Padova = University of Padua (Unipd), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de thermodynamique et physico-chimie métallurgiques (LTPCM), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Astronomia, Université Pierre et Marie Curie - Paris 6 (UPMC)-ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), and Department of Physics
Subjects: Redshifts, Astrophysics::Instrumentation and Methods for Astrophysics, [INFO]Computer Science [cs], Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Galaxies: IR, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Photometry: infrared, Astrophysics::Galaxy Astrophysics
Abstract: International audience; The catalog represents the final band-merged European Large-Area ISO Survey (ELAIS) Catalogue at 6.7, 15, 90 and 175\mu\m, and the associated data at U, g', r', i', Z, J, H, K and 20cm. Details about the origin of the survey, the observations, data reduction and optical identification are described in the paper. In addition to fluxes in the radio, infrared and optical passbands, spectroscopic redshifts are tabulated, where available. For the N1 and N2 areas, the Isaac Newton Telescope ugriz Wide Field Survey permits photometric redshifts to be estimated for galaxies and quasars. (2 data files).
Published: 2004

11. The Hawk-I UDS and GOODS Survey (HUGS): Survey design and deep K-band number counts.

Author: Fontana, A., Dunlop, J. S., Paris, D., Targett, T. A., Boutsia, K., Castellano, M., Galametz, A., Grazian, A., McLure, R., Merlin, E., Pentericci, L., Wuyts, S., Almaini, O., Caputi, K., Chary, R. -R., Cirasuolo, M., Conselice, C. J., Cooray, A., Daddi, E., and Dickinson, M.
Subjects: GALACTIC evolution, ASTRONOMICAL observations, ASTRONOMICAL surveys, DATA quality, ENERGY bands
Abstract: We present the results of a new, ultra-deep, near-infrared imaging survey executed with the Hawk-I imager at the ESO VLT, of which we make all the data (images and catalog) public. This survey, named HUGS (Hawk-I UDS and GOODS Survey), provides deep, high-quality imaging in the K and Y bands over the portions of the UKIDSS UDS and GOODS-South fields covered by the CANDELS HST WFC3/IR survey. In this paper we describe the survey strategy, the observational campaign, the data reduction process, and the data quality. We show that, thanks to exquisite image quality and extremely long exposure times, HUGS delivers the deepest K-band images ever collected over areas of cosmological interest, and in general ideally complements the CANDELS data set in terms of image quality and depth. In the GOODS-S field, the K-band observations cover the whole CANDELS area with a complex geometry made of 6 different, partly overlapping pointings, in order to best match the deep and wide areas of CANDELS imaging. In the deepest region (which includes most of the Hubble Ultra Deep Field) exposure times exceed 80 hours of integration, yielding a 1 - σ magnitude limit per square arcsec of '28.0 AB mag. The seeing is exceptional and homogeneous across the various pointings, confined to the range 0.38-0.43 arcsec. In the UDS field the survey is about one magnitude shallower (to match the correspondingly shallower depth of the CANDELS images) but includes also Y-band band imaging (which, in the UDS, was not provided by the CANDELS WFC3/IR imaging). In the K-band, with an average exposure time of 13 hours, and seeing in the range 0.37-0.43 arcsec, the 1 - σ limit per square arcsec in the UDS imaging is ≃27.3 AB mag. In the Y-band, with an average exposure time ≃8 h, and seeing in the range 0.45-0.5 arcsec, the imaging yields a 1 - σ limit per square arcsec of ≃28.3 AB mag. We show that the HUGS observations are well matched to the depth of the CANDELS WFC3/IR data, since the majority of even the faintest galaxies detected in the CANDELS H-band images are also detected in HUGS. Finally we present the K-band galaxy number counts produced by combining the HUGS data from the two fields. We show that the slope of the number counts depends sensitively on the assumed distribution of galaxy sizes, with potential impact on the estimated extra-galactic background light. [ABSTRACT FROM AUTHOR]
Published: 2014
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12. X-ray groups and clusters of galaxies in the Subaru–XMM Deep Field.

Author: Finoguenov, A., Watson, M. G., Tanaka, M., Simpson, C., Cirasuolo, M., Dunlop, J. S., Peacock, J. A., Farrah, D., Akiyama, M., Ueda, Y., Smolči, V., Stewart, G., Rawlings, S., van Breukelen, C., Almaini, O., Clewley, L., Bonfield, D. G., Jarvis, M. J., Barr, J. M., and Foucaud, S.
Subjects: GALAXY clusters, LOCAL Group (Astronomy), ASTRONOMY, RADIO sources (Astronomy), RADIO galaxies, METAPHYSICAL cosmology
Abstract: We present the results of a search for galaxy clusters in the Subaru–XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5–2 keV band of over one of the widest XMM–Newton contiguous raster surveys, covering an area of 1.3 deg2. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations. In addition, three sources are identified as X-ray counterparts of radio lobes, and in three further sources, an X-ray counterpart of the radio lobes provides a significant fraction of the total flux of the source. In the area covered by near-infrared data, our identification success rate achieves 86 per cent. We detect a number of radio galaxies within our groups, and for a luminosity-limited sample of radio galaxies we compute halo occupation statistics using a marked cluster mass function. We compare the cluster detection statistics in the SXDF with that in the literature and provide the modelling using the concordance cosmology combined with current knowledge of the X-ray cluster properties. The joint cluster is overpredicted by the model, and an agreement can be achieved through a reduction of the concordance σ8 value by 5 per cent. Having considered the and the X-ray luminosity function of clusters, we conclude that to pin down the origin of disagreement a much wider (50 deg2) survey is needed. [ABSTRACT FROM AUTHOR]
Published: 2010
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13. AzTEC half square degree survey of the SHADES fields – I. Maps, catalogues and source counts.

Author: Austermann, J. E., Dunlop, J. S., Perera, T. A., Scott, K. S., Wilson, G. W., Aretxaga, I., Hughes, D. H., Almaini, O., Chapin, E. L., Chapman, S. C., Cirasuolo, M., Clements, D. L., Coppin, K. E. K., Dunne, L., Dye, S., Eales, S. A., Egami, E., Farrah, D., Ferrusca, D., and Flynn, S.
Subjects: GALAXY formation, REDSHIFT, BOLOMETERS, ASTRONOMICAL observations, ASTROPHYSICS
Abstract: We present the first results from the largest deep extragalactic mm-wavelength survey undertaken to date. These results are derived from maps covering over 0.7 deg2, made at , using the AzTEC continuum camera mounted on the James Clerk Maxwell Telescope. The maps were made in the two fields originally targeted at with the Submillimetre Common-User Bolometer Array (SCUBA) in the SCUBA Half-Degree Extragalactic Survey (SHADES) project, namely the Lockman Hole East (mapped to a depth of 0.9–1.3 mJy rms) and the Subaru/ XMM–Newton Deep Field (mapped to a depth of 1.0–1.7 mJy rms). The wealth of existing and forthcoming deep multifrequency data in these two fields will allow the bright mm source population revealed by these new wide-area 1.1 mm images to be explored in detail in subsequent papers. Here, we present the maps themselves, a catalogue of 114 high-significance submillimetre galaxy detections, and a thorough statistical analysis leading to the most robust determination to date of the 1.1 mm source number counts. These new maps, covering an area nearly three times greater than the SCUBA SHADES maps, currently provide the largest sample of cosmological volumes of the high-redshift Universe in the mm or sub-mm. Through careful comparison, we find that both the Cosmic Evolution Survey (COSMOS) and the Great Observatories Origins Deep Survey (GOODS) North fields, also imaged with AzTEC, contain an excess of mm sources over the new 1.1 mm source-count baseline established here. In particular, our new AzTEC/SHADES results indicate that very luminous high-redshift dust enshrouded starbursts are 25–50 per cent less common than would have been inferred from these smaller surveys, thus highlighting the potential roles of cosmic variance and clustering in such measurements. We compare number count predictions from recent models of the evolving mm/sub-mm source population to these sub-mm bright galaxy surveys, which provide important constraints for the ongoing refinement of semi-analytic and hydrodynamical models of galaxy formation, and find that all available models overpredict the number of bright submillimetre galaxies found in this survey. [ABSTRACT FROM AUTHOR]
Published: 2010
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14. A pilot survey for KX QSOs in the UKIDSS Ultra Deep Survey Field.

Author: Smail, Ian, Sharp, Rob, Swinbank, A. M., Akiyama, M., Ueda, Y., Foucaud, S., Almaini, O., and Croom, S.
Subjects: QUASARS, SURVEYS, INFRARED radiation, ASTRONOMY, METAPHYSICAL cosmology
Abstract: We have undertaken a pilot survey for faint quasi-stellar objects (QSOs) in the UKIRT Infrared Deep Survey (UKIDSS) Ultra Deep Survey (UDS) Field using the KX selection technique. These observations exploit the very deep near-infrared and optical imaging of this field from United Kingdom Infrared Telescope (UKIRT) and Subaru to select candidate QSOs based on their VJK colours and morphologies. We determined redshifts for 426 candidates using the AAOmega spectrograph on the Anglo-Australian Telescope in service time. We identify 17 QSOs in this pilot survey at z= 1.57–3.29. We combine our sample with an X-ray-selected sample of QSOs in the same field (a large fraction of which also comply with our KX selection) to constrain the surface density of QSOs with K≤ 20, deriving limits on the likely surface density of 85–150 deg−2. We use the good image quality available from our near-infrared imaging to detect a spatially extended component of the QSO light which probably represents the host galaxies. We also use our sample to investigate routes to improve the selection of KX QSOs at faint limits in the face of the significant contamination by compact, foreground galaxies. The brightest examples from our combined QSO sample will be used in conjunction with a large Very Large Telescope VIMOS spectroscopic survey of high-redshift galaxies in this region to study the structures inhabited by gas, galaxies and growing supermassive black holes at high redshifts in the UKIDSS UDS. [ABSTRACT FROM AUTHOR]
Published: 2008
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15. On the evolution of clustering of 24-μm-selected galaxies.

Author: Magliocchetti, M., Cirasuolo, M., McLure, R. J., Dunlop, J. S., Almaini, O., Foucaud, S., De Zott, G., Simpson, C., and Sekiguchi, K.
Subjects: GALAXIES, SURVEYS, ASTRONOMY, STAR formation, GALAXY clusters
Abstract: This paper investigates the clustering properties of a complete sample of 1041 24-μm-selected sources brighter than in the overlapping region between the Spitzer Wide-Area Infrared Extragalactic (SWIRE) and UKIRT Infrared Deep Sky Survey (UKIDSS) Ultra Deep Survey (UDS) surveys. With the help of photometric redshift determinations we have concentrated on the two interval ranges z=[0.6–1.2] (low- z sample) and z≥ 1.6 (high- z sample) as it is in these regions were we expect the mid-infrared (IR) population to be dominated by intense dust-enshrouded activity such as star formation and black hole accretion. Investigations of the angular correlation function produce an amplitude A∼ 0.010 for the high- z sample and A∼ 0.0055 for the low- z one. The corresponding correlation lengths are and , showing that the high- z population is more strongly clustered. Comparisons with physical models for the formation and evolution of large-scale structure reveal that the high- z sources are exclusively associated with very massive haloes, comparable to those which locally host groups-to-clusters of galaxies and are very common within such (rare) structures. Conversely, lower z galaxies are found to reside in smaller haloes and to be very rare in such systems. On the other hand, mid-IR photometry shows that the low- z and high- z samples include similar objects and probe a similar mixture of active galactic nucleus (AGN) and star-forming galaxies. While recent studies have determined a strong evolution of the 24-μm luminosity function between z∼ 2 and 0, they cannot provide information on the physical nature of such an evolution. Our clustering results instead indicate that this is due to the presence of different populations of objects inhabiting different structures, as active systems at z≲ 1.5 are found to be exclusively associated with low-mass galaxies, while very massive sources appear to have concluded their active phase before this epoch. Finally, we note that the small-scale clustering data seem to require steep profiles for the distribution of galaxies within their haloes. This is suggestive of close encounters and/or mergers which could strongly favour both AGN and star formation activity. [ABSTRACT FROM AUTHOR]
Published: 2008
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16. The evolution of the near-infrared galaxy luminosity function and colour bimodality up to z≃ 2 from the UKIDSS Ultra Deep Survey Early Data Release.

Author: Cirasuolo, M., McLure, R. J., Dunlop, J. S., Almaini, O., Foucaud, S., Smail, Ian, Sekiguchi, K., Simpson, C., Eales, S., Dye, S., Watson, M. G., Page, M. J., and Hirst, P.
Subjects: GALAXY formation, STELLAR luminosity function, INFRARED astronomy, SURVEYS, METAPHYSICAL cosmology, ASTRONOMICAL research
Abstract: We present new results on the cosmological evolution of the near-infrared (near-IR) galaxy luminosity function (LF), derived from the analysis of a new sample of galaxies selected over an area of 0.6 deg2 from the Early Data Release of the UKIDSS Ultra Deep Survey (UDS). Our study has exploited the multiwavelength coverage of the UDS field provided by the new UKIDSS WFCAM K- and J-band imaging, the Subaru/ XMM–Newton Deep Survey and the Spitzer Wide-Area Infrared Extragalactic survey. The unique combination of large area and depth provided by this new survey minimizes the complicating effect of cosmic variance and has allowed us, for the first time, to trace the evolution of the brightest sources out to with good statistical accuracy. In agreement with previous studies, we find that the characteristic luminosity of the near-IR LF brightens by ≃1 mag between and , while the total density decreases by a factor of ≃2. Using the rest-frame colour to split the sample into red and blue galaxies, we confirm the classic luminosity-dependent colour bimodality at . However, the strength of the colour bimodality is found to be a decreasing function of redshift, and seems to disappear by . Due to the large size of our sample, we are able to investigate the differing cosmological evolution of the red and blue galaxy populations. It is found that the space density of the brightest red galaxies stays approximately constant with redshift, and that these sources dominate the bright end of the LF at redshifts . In contrast, the brightening of the characteristic luminosity and mild decrease in space density displayed by the blue galaxy population leads them to dominate the bright end of the LF at redshifts . [ABSTRACT FROM AUTHOR]
Published: 2007
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17. The UKIRT Infrared Deep Sky Survey (UKIDSS ).

Author: Lawrence, A., Warren, S. J., Almaini, O., Edge, A. C., Hambly, N. C., Jameson, R. F., Lucas, P., Casali, M., Adamson, A., Dye, S., Emerson, J. P., Foucaud, S., Hewett, P., Hirst, P., Hodgkin, S. T., Irwin, M. J., Lodieu, N., McMahon, R. G., Simpson, C., and Smail, I.
Subjects: SURVEYS, SKY, ASTRONOMICAL instruments, OPEN clusters of stars, SPACE sciences, MILKY Way
Abstract: We describe the goals, design, implementation, and initial progress of the UKIRT Infrared Deep Sky Survey (UKIDSS), a seven-year sky survey which began in 2005 May. UKIDSS is being carried out using the UKIRT Wide Field Camera (WFCAM), which has the largest étendue of any infrared astronomical instrument to date. It is a portfolio of five survey components covering various combinations of the filter set ZYJHK and H2. The Large Area Survey, the Galactic Clusters Survey, and the Galactic Plane Survey cover approximately 7000 deg2 to a depth of ; the Deep Extragalactic Survey covers 35 deg2 to , and the Ultra Deep Survey covers 0.77 deg2 to . Summed together UKIDSS is 12 times larger in effective volume than the 2MASS survey. The prime aim of UKIDSS is to provide a long-term astronomical legacy data base; the design is, however, driven by a series of specific goals – for example, to find the nearest and faintest substellar objects, to discover Population II brown dwarfs, if they exist, to determine the substellar mass function, to break the quasar barrier; to determine the epoch of re-ionization, to measure the growth of structure from to the present day, to determine the epoch of spheroid formation, and to map the Milky Way through the dust, to several kpc. The survey data are being uniformly processed. Images and catalogues are being made available through a fully queryable user interface – the WFCAM Science Archive ( ). The data are being released in stages. The data are immediately public to astronomers in all ESO member states, and available to the world after 18 months. Before the formal survey began, UKIRT and the UKIDSS consortia collaborated in obtaining and analysing a series of small science verification (SV) projects to complete the commissioning of the camera. We show some results from these SV projects in order to demonstrate the likely power of the eventual complete survey. Finally, using the data from the First Data Release, we assess how well UKIDSS is meeting its design targets so far. [ABSTRACT FROM AUTHOR]
Published: 2007
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18. The United Kingdom Infrared Telescope Infrared Deep Sky Survey First Data Release.

Author: Warren, S. J., Hambly, N. C., Dye, S., Almaini, O., Cross, N. J. G., Edge, A. C., Foucaud, S., Hewett, P. C., Hodgkin, S. T., Irwin, M. J., Jameson, R. F., Lawrence, A., Lucas, P. W., Adamson, A. J., Bandyopadhyay, R. M., Bryant, J., Collins, R. S., Davis, C. J., Dunlop, J. S., and Emerson, J. P.
Subjects: INFRARED telescopes, GALAXIES, ASTRONOMICAL instruments, ASTRONOMY, METAPHYSICAL cosmology
Abstract: The First Data Release (DR1) of the United Kingdom Infrared Telescope Infrared Deep Sky Survey (UKIDSS) took place on 2006 July 21. The UKIDSS is a set of five large near-infrared surveys, covering a complementary range of areas, depths and Galactic latitudes. The DR1 is the first large release of survey-quality data from the UKIDSS and includes 320 deg2 of multicolour data to (Vega) , complete (depending on the survey) in three to five bands from the set ZYJHK, together with 4 deg2 of deep JK data to an average depth . In addition, the release includes a similar quantity of data with incomplete filter coverage. In JHK, in regions of low extinction, the photometric uniformity of the calibration is better than 0.02 mag in each band. The accuracy of the calibration in ZY remains to be quantified, and the same is true of JHK in regions of high extinction. The median image full width at half-maximum across the data set is 0.82 arcsec. We describe changes since the Early Data Release in the implementation, pipeline and calibration, quality control, and archive procedures. We provide maps of the areas surveyed, and summarize the contents of each of the five surveys in terms of filters, areas and depths. The DR1 marks completion of 7 per cent of the UKIDSS seven-year goals. [ABSTRACT FROM AUTHOR]
Published: 2007
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19. The SCUBA Half-Degree Extragalactic Survey – II. Submillimetre maps, catalogue and number counts.

Author: Coppin, K., Chapin, E. L., Mortier, A. M. J., Scott, S. E., Borys, C., Dunlop, J. S., Halpern, M., Hughes, D. H., Pope, A., Scott, D., Serjeant, S., Wagg, J., Alexander, D. M., Almaini, O., Aretxaga, I., Babbedge, T., Best, P. N., Blain, A., Chapman, S., and Clements, D. L.
Subjects: METAPHYSICAL cosmology, COSMOGRAPHY, GALACTIC evolution, STARBURSTS, SUBMILLIMETER astronomy
Abstract: We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-μm SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/ XMM–Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720 arcmin2 with a rms noise level of about 2 mJy and have uncovered >100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We also find that a 850-μm survey complete down to 2 mJy would resolve 20–30 per cent of the far-infrared background into point sources. [ABSTRACT FROM AUTHOR]
Published: 2006
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20. The UKIRT Infrared Deep Sky Survey Early Data Release.

Author: Dye, S., Warren, S. J., Hambly, N. C., Cross, N. J. G., Hodgkin, S. T., Irwin, M. J., Lawrence, A., Adamson, A. J., Almaini, O., Edge, A. C., Hirst, P., Jameson, R. F., Lucas, P. W., van Breukelen, C., Bryant, J., Casali, M., Collins, R. S., Dalton, G. B., Davies, J. I., and Davis, C. J.
Subjects: INFRARED telescopes, ASTRONOMICAL photometry, ASTRONOMY, TELESCOPES
Abstract: This paper defines the UKIRT Infrared Deep Sky Survey (UKIDSS) Early Data Release (EDR). UKIDSS is a set of five large near-infrared surveys being undertaken with the United Kingdom Infrared Telescope Wide Field Camera (WFCAM). The programme began in 2005 May and has an expected duration of 7 yr. Each survey uses some or all of the broad-band filter complement ZY JHK. The EDR is the first public release of data to the European Southern Observatory (ESO) community. All worldwide releases occur after a delay of 18 months from the ESO release. The EDR provides a small sample data set, ∼50 deg2 (about 1 per cent of the whole of UKIDSS), that is a lower limit to the expected quality of future survey data releases. In addition, an EDR+ data set contains all EDR data plus extra data of similar quality, but for areas not observed in all of the required filters (amounting to ∼220 deg2). The first large data release, DR1, will occur in mid-2006. We provide details of the observational implementation, the data reduction, the astrometric and photometric calibration and the quality control procedures. We summarize the data coverage and quality (seeing, ellipticity, photometricity, depth) for each survey and give a brief guide to accessing the images and catalogues from the WFCAM Science Archive. [ABSTRACT FROM AUTHOR]
Published: 2006
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21. Galaxy clusters at 0.6 < z < 1.4 in the UKIDSS Ultra Deep Survey Early Data Release.

Author: van Breukelen, C., Clewley, L., Bonfield, D. G., Rawlings, S., Jarvis, M. J., Barr, J. M., Foucaud, S., Almaini, O., Cirasuolo, M., Dalton, G., Dunlop, J. S., Edge, A. C., Hirst, P., McLure, R. J., Page, M. J., Sekiguchi, K., Simpson, C., Smail, I., and Watson, M. G.
Subjects: GALAXY clusters, INFRARED telescopes, ASTRONOMICAL photometry, ACTIVE galactic nuclei, STAR formation, REDSHIFT, ASTROPHYSICS
Abstract: We present the first cluster catalogue extracted from the UKIRT Infrared Deep Sky Survey (UKIDSS) Early Data Release. The catalogue is created using UKIDSS Ultra Deep Survey infrared J and K data combined with 3.6- and 4.5-μm Spitzer bands and optical BVRi′ z′ imaging from the Subaru Telescope over 0.5 deg2 in the Subaru XMM–Newton Deep Field. We have created a new cluster detection algorithm, based on the friends-of-friends and Voronoi tessellation methods, which utilizes probability distribution functions derived from a photometric redshift analysis. We employ mock catalogues to understand the selection effects and contamination associated with the algorithm. The cluster catalogue contains 13 clusters at redshifts with luminosities , corresponding to masses for . The measured sky surface density of for high-redshift , massive clusters is precisely in line with theoretical predictions presented by Kneissl et al. [ABSTRACT FROM AUTHOR]
Published: 2006
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22. Mid-infrared sources in the ELAIS Deep X-ray Survey.

Author: Manners, J. C., Serjeant, S., Bottinelli, S., Vaccari, M., Franceschini, A., Perez-Fournon, I., Gonzalez-Solares, E., Willott, C. J., Johnson, O., Almaini, O., Rowan-Robinson, M., and Oliver, S.
Subjects: INFRARED sources, LIGHT sources, STAR formation, GALACTIC cosmic rays, GALACTIC X-ray sources, GALAXIES
Abstract: We present a cross-correlation of the European Large AreaInfrared Space Observatory(ISO) survey (ELAIS) with the ELAIS Deep X-ray Survey of the N1 and N2 fields. There are sevenChandrapoint sources with matches in the ELAIS Final Analysis 15-μm catalogue, out of a total of 28 extragalacticISOsources present in theChandrafields. Five of these are consistent with active galactic nuclei (AGN) giving an AGN fraction of∼19 per cent in the 15-μm flux range 0.8–6 mJy. We have co-added the hard X-ray fluxes of the individually undetectedISOsources and find a low significance detection consistent with star formation in the remaining population. We combine our point source cross-correlation fraction with theXMM–Newtonobservations of the Lockman Hole andChandraobservations of theHubble Deep FieldNorth to constrain source count models of the mid-infrared galaxy population. The low dust-enshrouded AGN fraction in ELAIS implied by the number of cross-identifications between the ELAIS mid-infrared sample and theChandrapoint sources is encouraging for the use of mid-infrared surveys to constrain the cosmic star formation history, provided there are not further large undetected populations of Compton-thick AGN. [ABSTRACT FROM AUTHOR]
Published: 2004
Full Text: View/download PDF

23. The ELAIS deep X-ray survey – I. Chandra source catalogue and first results.

Author: Manners, J. C., Johnson, O., Almaini, O., Willott, C. J., Gonzalez-Solares, E., Lawrence, A., Mann, R. G., Perez-Fournon, I., Dunlop, J. S., McMahon, R. G., Oliver, S. J., Rowan-Robinson, M., and Serjeant, S.
Subjects: GALAXIES, ASTRONOMY
Abstract: ABSTRACT We present an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. Here we present the Chandra source catalogues along with an analysis of source counts, hardness ratios and optical classifications. A total of 233 X-ray point sources are detected in addition to two soft extended sources, which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which we attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. [ABSTRACT FROM AUTHOR]
Published: 2003
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24. The SCUBA 8-mJy survey – II. Multiwavelength analysis of bright submillimetre sources.

Author: Fox, M. J., Efstathiou, A., Rowan-Robinson, M., Dunlop, J. S., Scott, S., Serjeant, S., Mann, R. G., Oliver, S., Ivison, R. J., Blain, A., Almaini, O., Hughes, D., Willott, C. J., Longair, M., Lawrence, A., and Peacock, J. A.
Subjects: GALAXIES, SURVEYS, METAPHYSICAL cosmology
Abstract: We present the results of a multiwavelength study of the 19 most significant submillimetre (submm) sources detected in the SCUBA 8-mJy survey. As described in Scott et al. , this survey covers ≃260 arcmin[sup 2] using the submillimetre camera SCUBA, to a limiting source detection limit S[sub 850 μm]≃8 mJy . One advantage of this relatively bright flux-density limit is that accurate astrometric positions are potentially achievable for every source using existing radio and/or millimetre-wave interferometers. However, an associated advantage is that spectral energy distribution (SED) based redshift constraints should be more powerful than in fainter submm surveys. Here we therefore exploit the parallel SCUBA 450-μm data, in combination with existing radio and Infrared Space Observatory (ISO) data at longer and shorter wavelengths to set constraints on the redshift of each source. We also analyse new and existing optical and near-infrared imaging of our SCUBA survey fields to select potential identifications consistent with these constraints. Our derived SED-based redshift constraints, and the lack of statistically significant associations with even moderately bright galaxies allow us to conclude that all 19 sources lie at z>1 , and at least half of them apparently lie at z>2 . [ABSTRACT FROM AUTHOR]
Published: 2002
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25. The European Large Area ISO Survey – I. Goals, definition and observations.

Author: Oliver, S., Rowan-Robinson, M., Alexander, D.M., Almaini, O., Balcells, M., Baker, A.C., Barcons, X., Barden, M., Bellas-Velidis, I., Cabrera-Guerra, F., Carballo, R., Cesarsky, C.J., Ciliegi, P., Clements, D.L., Crockett, H., Danese, L., Dapergolas, A., Drolias, B., Eaton, N., and Efstathiou, A.
Subjects: GALAXIES, SURVEYS, STAR formation
Abstract: We describe the European Large Area ISO Survey (ELAIS). ELAIS was the largest single Open Time project conducted by ISO, mapping an area of 12 deg[sup 2] at 15 μm with ISOCAM and at 90 μm with ISOPHOT. Secondary surveys in other ISO bands were undertaken by the ELAIS team within the fields of the primary survey, with 6 deg[sup 2] being covered at 6.7 μm and 1 deg[sup 2] at 175 μm. This paper discusses the goals of the project and the techniques employed in its construction, as well as presenting details of the observations carried out, the data from which are now in the public domain. We outline the ELAIS ‘preliminary analysis’ which led to the detection of over 1000 sources from the 15 and 90-μm surveys (the majority selected at 15 μm with a flux limit of ∼3 mJy), to be fed into a ground-based follow-up campaign, as well as a programme of photometric observations of detected sources using both ISOCAM and ISOPHOT. We detail how the ELAIS survey complements other ISO surveys in terms of depth and areal coverage, and show that the extensive multi-wavelength coverage of the ELAIS fields resulting from our concerted and on-going follow-up programme has made these regions amongst the best studied areas of their size in the entire sky, and, therefore, natural targets for future surveys. This paper accompanies the release of extremely reliable subsets of the ‘preliminary analysis’ products. Subsequent papers in this series will give further details of our data reduction techniques, reliability and completeness estimates and present the 15- and 90-μm number counts from the ‘preliminary analysis’, while a further series of papers will discuss in detail the results from the ELAIS ‘final analysis’, as well as from the follow-up programme. [ABSTRACT FROM AUTHOR]
Published: 2000
Full Text: View/download PDF

26. The European Large Area ISO Survey - I. Goals, definition and observations

Author: Oliver, S., Rowan-Robinson, M., Alexander, D. M., Almaini, O., Balcells, M., Baker, A. C., Barcons, X., Barden, M., Bellas-Velidis, I., Cabrera-Guerra, F., Carballo, R., Cesarsky, C. J., Ciliegi, P., Clements, D. L., Crockett, H., Danese, L., Dapergolas, A., Drolias, B., Eaton, N., Efstathiou, A., Egami, E., Elbaz, D., Fadda, D., Fox, M., Franceschini, A., Genzel, R., Goldschmidt, P., Graham, M., Gonzalez-Serrano, J. I., Gonzalez-Solares, E. A., Granato, G. L., Gruppioni, C., Herbstmeier, U., Héraudeau, P., Joshi, M., Kontizas, E., Kontizas, M., Kotilainen, J. K., Kunze, D., La Franca, F., Lari, C., Lawrence, A., Lemke, D., Linden-Vørnle, M. J. D., Mann, R. G., Márquez, I., Masegosa, J., Mattila, K., Mcmahon, R. G., Miley, G., Missoulis, V., Mobasher, B., Morel, T., Nørgaard-Nielsen, H., Omont, A., Papadopoulos, P., Perez-Fournon, I., Puget, J. -L, Rigopoulou, D., Rocca-Volmerange, B., Serjeant, S., Silva, L., Sumner, T., Surace, C., Vaisanen, P., Werf, P. P., Verma, A., Vigroux, L., Montserrat Villar Martin, Willott, C. J., Laboratoire de Physico-Chimie des Polymères et des Milieux Dispersés (PPMD), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, AUTRES, Space Telescope Science Institute (STSci), Laboratoire de thermodynamique et physico-chimie métallurgiques (LTPCM), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Physics [Oxford], University of Oxford, Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Centro de Fisica de Plasmas (GoLP), Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), Imperial College London, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Oxford Astrophysics, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Steward Observatory, University of Arizona, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National Polytechnique de Grenoble (INPG)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Universidad de Cantabria, Université Pierre et Marie Curie - Paris 6 (UPMC)-ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, University of Oxford [Oxford], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: GALAXIES: EVOLUTION, active [Galaxies], 010504 meteorology & atmospheric sciences, media_common.quotation_subject, GALAXIES: STARBURST, FOS: Physical sciences, Astrophysics, Surveys, 01 natural sciences, GALAXIES: ACTIVE, galaxies [Infrared], 0103 physical sciences, [INFO]Computer Science [cs], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Astrophysics (astro-ph), Astronomy and Astrophysics, evolution [Galaxies], Square degree, INFRARED: GALAXIES, starburst [Galaxies], Space and Planetary Science, Sky, stars [Infrared], INFRARED: STARS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cartography, SURVEYS
Abstract: We describe the European Large Area ISO Survey (ELAIS). ELAIS was the largest single Open Time project conducted by ISO, mapping an area of 12 square degrees at 15mu with ISO-CAM and at 90mu with ISO-PHOT. Secondary surveys in other ISO bands were undertaken by the ELAIS team within the fields of the primary survey, with 6 square degrees being covered at 6.7mu and 1 square degree at 175mu. This paper discusses the goals of the project and the techniques employed in its construction, as well as presenting details of the observations carried out, the data from which are now in the public domain. We outline the ELAIS ``Preliminary Analysis'' which led to the detection of over 1000 sources from the 15 and 90 mu surveys (the majority selected at 15mu with a flux limit of ~3 mJy), to be fed into a ground-based follow-up campaign, as well as a programme of photometric observations of detected sources using both ISO-CAM and ISO-PHOT. We detail how the ELAIS survey complements other ISO surveys in terms of depth and areal coverage, and show that the extensive multi-wavelength coverage of the ELAIS fields resulting from our concerted and on-going follow-up programme has made these regions amongst the best studied areas of their size in the entire sky, and, therefore, natural targets for future surveys. This paper accompanies the release of extremely reliable sub-sets of the ``Preliminary Analysis'' products. Subsequent papers in this series will give further details of our data reduction techniques, reliability & completeness estimates and present the 15 and 90 nu number counts from the ``Preliminary Analysis'', while a further series of papers will discuss in detail the results from the ELAIS ``Final Analysis'', as well as from the follow-up programme., 23 pages 16 Figures, MNRAS accepted, see also http://athena.ph.ic.ac.uk/, revisions ELAIS consortium added to authors above, one figure un-inverted

27. The VANDELS ESO public spectroscopic survey

Author: Nimish P. Hathi, Michele Moresco, Jennifer M. Lotz, Seock-Sam Kim, Lidia Tasca, Andrea Grazian, Intae Jung, Adriano Fontana, Casey Papovich, William G. Hartley, Kirpal Nandra, Emanuela Pompei, S. Bardelli, R. Begley, Mauro Giavalisco, Paola Santini, H. C. Ferguson, Andrea Cimatti, J. S. Dunlop, Lucia Guaita, H. Mendez-Hernandez, Christina C. Williams, Giovanni Cresci, A. C. Carnall, A. Saxena, Adriana Gargiulo, Paolo Cassata, A. Iovino, C. Caputi, D. Maccagni, Stephane Charlot, Michele Cirasuolo, Johan P. U. Fynbo, Stefano Cristiani, Fabrizio Fiore, L. Pentericci, Guido Roberts-Borsani, E. Curtis-Lake, M. Longhetti, Manuela Magliocchetti, Matt J. Jarvis, M. Mignoli, Y. Khusanova, Paola Popesso, Annalisa Citro, Mara Salvato, Ricardo Amorín, Lucia Pozzetti, Olga Cucciati, Fergus Cullen, Pascale Hibon, Fernando Buitrago, Daniel P. Stark, Corentin Schreiber, M. Fumana, P. Franzetti, Jairo Méndez-Abreu, E. Zucca, R. C. Thomas, Filippo Mannucci, Ross J. McLure, Mark Dickinson, K. Matsuoka, M. Franco, O. Le Fèvre, Daniel Schaerer, Steve Finkelstein, M. Bolzonella, Fabio Fontanot, David J. Rosario, Eric F. Bell, Marco Castellano, A. Calabrò, Antonis Georgakakis, Mario Nonino, G. Vietri, Maurilio Pannella, G. Brammer, Marcella Brusa, David T. Maltby, Stéphanie Juneau, Bianca Garilli, Anton M. Koekemoer, Angela Bongiorno, Vivienne Wild, Giovanni G. Fazio, David Elbaz, Margherita Talia, D. J. McLeod, M. Scodeggio, Alberto Saldana-Lopez, M. Hamadouche, Italo Balestra, Omar Almaini, G. Zamorani, Eros Vanzella, Rebecca A. A. Bowler, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Garilli B., McLure R., Pentericci L., Franzetti P., Gargiulo A., Carnall A., Cucciati O., Iovino A., Amorin R., Bolzonella M., Bongiorno A., Castellano M., Cimatti A., Cirasuolo M., Cullen F., Dunlop J., Elbaz D., Finkelstein S., Fontana A., Fontanot F., Fumana M., Guaita L., Hartley W., Jarvis M., Juneau S., Maccagni D., McLeod D., Nandra K., Pompei E., Pozzetti L., Scodeggio M., Talia M., Calabro A., Cresci G., Fynbo J.P.U., Hathi N.P., Hibon P., Koekemoer A.M., Magliocchetti M., Salvato M., Vietri G., Zamorani G., Almaini O., Balestra I., Bardelli S., Begley R., Brammer G., Bell E.F., Bowler R.A.A., Brusa M., Buitrago F., Caputi C., Cassata P., Charlot S., Citro A., Cristiani S., Curtis-Lake E., Dickinson M., Fazio G., Ferguson H.C., Fiore F., Franco M., Georgakakis A., Giavalisco M., Grazian A., Hamadouche M., Jung I., Kim S., Khusanova Y., Le Fevre O., Longhetti M., Lotz J., Mannucci F., Maltby D., Matsuoka K., Mendez-Hernandez H., Mendez-Abreu J., Mignoli M., Moresco M., Nonino M., Pannella M., Papovich C., Popesso P., Roberts-Borsani G., Rosario D.J., Saldana-Lopez A., Santini P., Saxena A., Schaerer D., Schreiber C., Stark D., Tasca L.A.M., Thomas R., Vanzella E., Wild V., Williams C., Zucca E., University of St Andrews. School of Physics and Astronomy, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: SELECTION, Galaxies: fundamental parameter, Astrophysics, I, Surveys, 01 natural sciences, observations/surveys/catalogs [Cosmology], Cosmology: observation, Cosmology: Observations, Spectral line, statistics [Galaxies], DATA-REDUCTION, QB Astronomy, Galaxies: distances and redshift, Galaxies: Fundamental Parameters, 010303 astronomy & astrophysics, QC, QB, REDSHIFT SURVEY, Physics, observations [cosmology], Catalogs, Cosmology: observations, Galaxies: distances and redshifts, Galaxies: fundamental parameters, Galaxies: statistics, Galaxies: Statistics, fundamental parameters [Galaxies], astro-ph.CO, Catalog, X-RAY-PROPERTIES, Data release, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: Distances and Redshifts, surveys, 0103 physical sciences, STAR-FORMING GALAXIES, distances and redshifts [Galaxies], Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Galaxies: statistic, Astronomy and Astrophysics, DAS, VLT DEEP SURVEY, Astrophysics - Astrophysics of Galaxies, EVOLUTION, STELLAR, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), QUIESCENT GALAXIES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract: VANDELS is an ESO Public Spectroscopic Survey designed to build a sample of high signal to noise, medium resolution spectra of galaxies at redshift between 1 and 6.5. Here we present the final Public Data Release of the VANDELS Survey, comprising 2087 redshift measurements. We give a detailed description of sample selection, observations and data reduction procedures. The final catalogue reaches a target selection completeness of 40% at iAB = 25. The high Signal to Noise ratio of the spectra (above 7 in 80% of the spectra) and the dispersion of 2.5�� allowed us to measure redshifts with high precision, the redshift measurement success rate reaching almost 100%. Together with the redshift catalogue and the reduced spectra, we also provide optical mid-IR photometry and physical parameters derived through SED fitting. The observed galaxy sample comprises both passive and star forming galaxies covering a stellar mass range 8.3< Log(M*/Msolar), 16 pages, 13 figures, accepted for publication in Astronomy & Astrophysics
Published: 2021

28. The VANDELS ESO public spectroscopic survey

Author: H. Mendez-Hernandez, Matt J. Jarvis, Mark Dickinson, D. Maccagni, Lucia Pozzetti, Ricardo Amorín, Christina C. Williams, B. Garilli, Eros Vanzella, David T. Maltby, A. Iovino, Omar Almaini, Marco Castellano, Antonis Georgakakis, Italo Balestra, Daniel Schaerer, M. Mignoli, Y. Khusanova, D. P. Rosario, Steve Finkelstein, P. Popesso, Andrea Grazian, Marcella Brusa, Anton M. Koekemoer, Maurilio Pannella, S. Juneau, Ross J. McLure, Michele Cirasuolo, Vivienne Wild, P. Santini, Nimish P. Hathi, K. Matsuoka, Seock-Sam Kim, Giovanni Cresci, Kirpal Nandra, Jairo Méndez-Abreu, Fabio Fontanot, F. Mannucci, A. C. Carnall, Laura Pentericci, Eric F. Bell, P. Franzetti, Fernando Buitrago, Michele Moresco, D. J. McLeod, Andrea Cimatti, Adriana Gargiulo, James Dunlop, E. Curtis-Lake, Rebecca A. A. Bowler, S. de Barros, Fabrizio Fiore, M. Bolzonella, D. Elbaz, Johan P. U. Fynbo, Giovanni G. Fazio, Margherita Talia, V. Sommariva, Marco Scodeggio, Stefano Cristiani, Jennifer M. Lotz, S. Bardelli, Mario Nonino, M. Giavalisco, Corentin Schreiber, Mara Salvato, Henry C. Ferguson, Audrey Galametz, E. Zucca, O. Le Fevre, Angela Bongiorno, M. Fumana, L. A. M. Tasca, Daniel P. Stark, Nathan Bourne, F. Marchi, M. Franco, W. G. Hartley, Stéphane Charlot, Adriano Fontana, Paolo Cassata, E. Mármol-Queraltó, W. Karman, Karina Caputi, Tommaso Treu, R. Thomas, Casey Papovich, Emanuela Pompei, O. Cucciati, Alice Mortlock, Annalisa Citro, Fergus Cullen, Intae Jung, G. Zamorani, Lucia Guaita, Astronomy, McLure, R. J., Pentericci, L., Cimatti, A., Dunlop, J. S., Elbaz, D., Fontana, A., Nandra, K., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cirasuolo, M., Cucciati, O., Cullen, F., De Barros, S., Finkelstein, S. L., Fontanot, F., Franzetti, P., Fumana, M., Gargiulo, A., Garilli, B., Guaita, L., Hartley, W. G., Iovino, A., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Mármol-Queraltó, E., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astronomico di Bologna (OABO), Department of Surgery, Santi Giovanni e Paolo Hospital, Association de Coordination Technique Agricole (ACTA), Space Telescope Science Institute (STSci), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Department of Agronomy, Food, Natural Resources, Animals and the Environment (DAFNAE), Universita degli Studi di Padova, Institute for General Botany, Johannes Gutenberg - Universität Mainz (JGU), Les instituts techniques agricoles (Acta), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository
Subjects: Active galactic nucleus, Stellar population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Survey, 010303 astronomy & astrophysics, Galaxies: high, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Galaxies: evolution, Galaxies: star formation, Surveys, Chandra Deep Field South, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract: VANDELS is a uniquely-deep spectroscopic survey of high-redshift galaxies with the VIMOS spectrograph on ESO's Very Large Telescope (VLT). The survey has obtained ultra-deep optical (0.48 < lambda < 1.0 micron) spectroscopy of ~2100 galaxies within the redshift interval 1.0 < z < 7.0, over a total area of ~0.2 sq. degrees centred on the CANDELS UDS and CDFS fields. Based on accurate photometric redshift pre-selection, 85% of the galaxies targeted by VANDELS were selected to be at z>=3. Exploiting the red sensitivity of the refurbished VIMOS spectrograph, the fundamental aim of the survey is to provide the high signal-to-noise ratio spectra necessary to measure key physical properties such as stellar population ages, masses, metallicities and outflow velocities from detailed absorption-line studies. Using integration times calculated to produce an approximately constant signal-to-noise ratio (20 < t_int < 80 hours), the VANDELS survey targeted: a) bright star-forming galaxies at 2.4 < z < 5.5, b) massive quiescent galaxies at 1.0 < z < 2.5, c) fainter star-forming galaxies at 3.0 < z < 7.0 and d) X-ray/Spitzer-selected active galactic nuclei and Herschel-detected galaxies. By targeting two extragalactic survey fields with superb multi-wavelength imaging data, VANDELS will produce a unique legacy data set for exploring the physics underpinning high-redshift galaxy evolution. In this paper we provide an overview of the VANDELS survey designed to support the science exploitation of the first ESO public data release, focusing on the scientific motivation, survey design and target selection., 19 pages, 9 figures, accepted for publication in MNRAS
Published: 2018

29. The VANDELS ESO public spectroscopic survey: observations and first data release

Author: O. Cucciati, Andrea Grazian, E. Zucca, Y. Khusanova, Emma Curtis-Lake, A. Iovino, Stéphane Charlot, R. J. McLure B. Garilli, James Dunlop, Adriana Gargiulo, Johan P. U. Fynbo, Alice Mortlock, Mara Salvato, E. Mármol-Queraltó, Nimish P. Hathi, Seock-Sam Kim, L. A. M. Tasca, Fabrizio Fiore, Italo Balestra, Kirpal Nandra, A. Georgakakis, Emanuela Pompei, D. Elbaz, Anton M. Koekemoer, S. L. Finkelstein, F. Marchi, M. Franco, Maurilio Pannella, Tommaso Treu, Audrey Galametz, Corentin Schreiber, H. Mendez-Hernandez, Andrea Cimatti, P. Popesso, M. Fumana, Giovanni G. Fazio, S. Cristiani, Angela Bongiorno, David J. Rosario, Laura Pentericci, Marco Castellano, Piero Rosati, Vivienne Wild, Giovanni Cresci, A. C. Carnall, C. Caputi, M. Giavalisco, Paolo Cassata, Lucia Pozzetti, Marcella Brusa, M. Bolzonella, R. C. Thomas, Margherita Talia, D. Maccagni, S. Bardelli, W. Karman, S. DeBarros, K. Matsuoka, H. C. Ferguson, Jennifer M. Lotz, F. Fontanot, Adriano Fontana, C. Papovich, W. G. Hartley, Michele Moresco, Eros Vanzella, David T. Maltby, Omar Almaini, S. Juneau, Rebecca A. A. Bowler, Daniel Schaerer, Daniel P. Stark, Nathan Bourne, S. M. Faber, D. J. McLeod, Ricardo Amorín, Michele Cirasuolo, P. Franzetti, Fernando Buitrago, O. Le Fevre, Annalisa Citro, Mario Nonino, Fergus Cullen, Intae Jung, G. Zamorani, Eric F. Bell, Lucia Guaita, Christina C. Williams, V. Sommariva, Marco Scodeggio, M. Mignoli, Matt J. Jarvis, Mark Dickinson, P. Santini, Jairo Méndez-Abreu, F. Mannucci, ITA, USA, GBR, FRA, DEU, INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Milano (OAM), INAF - Osservatorio Astronomico di Bologna (OABO), INAF - Osservatorio Astronomico di Brera (OAB), Università di Bologna, Dipartimento di Astronomia, Università di Bologna [Bologna] (UNIBO), INAF - Osservatorio Astronomico di Bologna (OAB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), CNR-INFM CRS-Soft, c/o Dipartimento di Fisica, CNR-INFM CRS-Soft, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), INAF-IASF Milano, European Southern Observatory (ESO), University of Bologna, INAF - Osservatorio Astronomico di Trieste (OAT), Dipartimento di Fisica e Astronomia [Bologna], University of Groningen [Groningen], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Osservatorio Astronomico (INAF), NOAO, Max-Planck-Institut für Extraterrestrische Physik (MPE), Department of Astronomy [Amherst], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Space Telescope Science Institute (STSci), Department of computer science, Kyushu Institute of Technology, University of Texas-Pan American (UTPA), University of Texas-Pan, Excellence Cluster Universe, Technische Universität München [München] (TUM), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), National Optical Astronomy Observatory (NOAO), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Bologna/Università di Bologna, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Kyushu Institute of Technology (Kyutech), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Pentericci, L., McLure, R. J., Garilli, B., Cucciati, O., Franzetti, P., Iovino, A., Amorin, R., Bolzonella, M., Bongiorno, A., Carnall, A. C., Castellano, M., Cimatti, A., Cirasuolo, M., Cullen, F., De Barros, S., Dunlop, J. S., Elbaz, D., Finkelstein, S. L., Fontana, A., Fontanot, F., Fumana, M., Gargiulo, A., Guaita, L., Hartley, W. G., Jarvis, M. J., Juneau, S., Karman, W., Maccagni, D., Marchi, F., Marmol-Queralto, E., Nandra, K., Pompei, E., Pozzetti, L., Scodeggio, M., Sommariva, V., Talia, M., Almaini, O., Balestra, I., Bardelli, S., Bell, E. F., Bourne, N., Bowler, R. A. A., Brusa, M., Buitrago, F., Caputi, K. I., Cassata, P., Charlot, S., Citro, A., Cresci, G., Cristiani, S., Curtis-Lake, E., Dickinson, M., Fazio, G. G., Ferguson, H. C., Fiore, F., Franco, M., Fynbo, J. P. U., Galametz, A., Georgakakis, A., Giavalisco, M., Grazian, A., Hathi, N. P., Jung, I., Kim, S., Koekemoer, A. M., Khusanova, Y., Le Fèvre, O., Lotz, J. M., Mannucci, F., Maltby, D. T., Matsuoka, K., McLeod, D. J., Mendez-Hernandez, H., Mendez-Abreu, J., Mignoli, M., Moresco, M., Mortlock, A., Nonino, M., Pannella, M., Papovich, C., Popesso, P., Rosario, D. P., Salvato, M., Santini, P., Schaerer, D., Schreiber, C., Stark, D. P., Tasca, L. A. M., Thomas, R., Treu, T., Vanzella, E., Wild, V., Williams, C. C., Zamorani, G., Zucca, E., Amorin Barbieri, Ricardo [0000-0001-5758-1000], and Apollo - University of Cambridge Repository
Subjects: media_common.quotation_subject, REDSHIFT, Galaxies: fundamental parameter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, 0103 physical sciences, Galaxy formation and evolution, fundamental parameters [galaxies], QB Astronomy, Survey, Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Galaxies: high-redshift, Surveys, Astronomy and Astrophysics, Space and Planetary Science, 010303 astronomy & astrophysics, Spectrograph, evolution [galaxies], QC, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, media_common, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, galaxies: fundamental parameters, 3rd-DAS, Astronomy and Astrophysic, galaxies: general, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Universe, Data set, GALAXIES, QC Physics, Sky, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), VIMOS, galaxies: evolution, high-redshift [galaxies], Data reduction, general [galaxies]
Abstract: This paper describes the observations and the first data release (DR1) of the ESO public spectroscopic survey "VANDELS, a deep VIMOS survey of the CANDELS CDFS and UDS fields". VANDELS' main targets are star-forming galaxies at 2.4, Comment: Submitted to A&A
Published: 2018

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29 results on '"Almaini, O"'

1. Increasing AGN sample completeness using long-term near-infrared variability.

2. STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS

3. The VANDELS ESO public spectroscopic survey

4. Infrared lags in the light curves of AGNs measured using a deep survey.

5. The VANDELS ESO spectroscopic survey

6. The SCUBA-2 Cosmology Legacy Survey: 850 ?m maps, catalogues and number counts

7. Long-term NIR variability in the UKIDSS Ultra Deep Survey: a new probe of AGN activity at high redshift.

8. The UKIRT Infrared Deep Sky Survey Early Data Release

9. The SCUBA-2 Cosmology Legacy Survey: 850 µm maps, catalogues and number counts.

10. VizieR Online Data Catalog: ELAIS: final band-merged catalogue (Rowan-Robinson+, 2004)

11. The Hawk-I UDS and GOODS Survey (HUGS): Survey design and deep K-band number counts.

12. X-ray groups and clusters of galaxies in the Subaru–XMM Deep Field.

13. AzTEC half square degree survey of the SHADES fields – I. Maps, catalogues and source counts.

14. A pilot survey for KX QSOs in the UKIDSS Ultra Deep Survey Field.

15. On the evolution of clustering of 24-μm-selected galaxies.

16. The evolution of the near-infrared galaxy luminosity function and colour bimodality up to z≃ 2 from the UKIDSS Ultra Deep Survey Early Data Release.

17. The UKIRT Infrared Deep Sky Survey (UKIDSS ).

18. The United Kingdom Infrared Telescope Infrared Deep Sky Survey First Data Release.

19. The SCUBA Half-Degree Extragalactic Survey – II. Submillimetre maps, catalogue and number counts.

20. The UKIRT Infrared Deep Sky Survey Early Data Release.

21. Galaxy clusters at 0.6 < z < 1.4 in the UKIDSS Ultra Deep Survey Early Data Release.

22. Mid-infrared sources in the ELAIS Deep X-ray Survey.

23. The ELAIS deep X-ray survey – I. Chandra source catalogue and first results.

24. The SCUBA 8-mJy survey – II. Multiwavelength analysis of bright submillimetre sources.

25. The European Large Area ISO Survey – I. Goals, definition and observations.

26. The European Large Area ISO Survey - I. Goals, definition and observations

27. The VANDELS ESO public spectroscopic survey

28. The VANDELS ESO public spectroscopic survey

29. The VANDELS ESO public spectroscopic survey: observations and first data release

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29 results on '"Almaini, O"'

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