HAWK-I: the high-acuity wide-field <i>K</i>-band imager  for the ESO Very Large Telescope

Kissler-Patig, M.; Pirard, Jeff; Casali, M.; Moorwood, A. F. M.; Ageorges, N.; Oliveira, Catarina Alves de; Baksai, Pedro; Bedin, L. R.; Bendek, Eduardo; Biereichel, P.; Délabre, Bernard; Dorn, Reinhold J.; Esteves, R.; Finger, Gert; Gojak, D.; Huster, Gotthard; Jung, Yves; Kiekebush, Mario; Klein, Barbara; Koch, Franz; Lizon, Jean Louis; Mehrgan, Leander; Petr-Gotzens, M. G.; Pritchard, J.; Selman, F.; Stegmeier, Jörg

doi:10.1051/0004-6361:200809910

Cited by 139 publications

(92 citation statements)

References 7 publications

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“…Tran) using HAWK-I (Kissler-Patig et al 2008) on the ESO Very Large Telescope (VLT). HAWK-I is a near-IR camera comprising four Hawaii-2 2048 × 2048 pixel detectors separated by a gap of ∼ 15 arcsec.…”

Section: Broad-band Photometrymentioning

confidence: 99%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a comprehensive picture of the Cl 0218.3−0510 protocluster at z = 1.623 across 10 co-moving Mpc. Using filters that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies we obtain precise photometric redshifts resulting in a protocluster galaxy sample that is 89 ± 5% complete and has a contamination of only 12 ± 5%. Both star forming and quiescent protocluster galaxies are located allowing us to map the structure of the forming cluster for the first time. The protocluster contains 6 galaxy groups, the largest of which is the nascent cluster. Only a small minority of the protocluster galaxies are in the nascent cluster (11%) or in the other galaxy groups (22%), as most protocluster galaxies reside between the groups. Unobscured star forming galaxies predominantly reside between the protocluster's groups, whereas red galaxies make up a large fraction of the groups' galactic content, so observing the protocluster through only one of these types of galaxies results in a biased view of the protocluster's structure. The structure of the protocluster reveals how much mass is available for the future growth of the cluster and we use the Millennium Simulation, scaled to a Planck cosmology, to predict that Cl 0218.3−0510 will evolve into a 2.7 +3.9 −1.7 × 10 14 M ⊙ cluster by the present day.

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Section: Broad-band Photometrymentioning

confidence: 99%

The structure and evolution of a forming galaxy cluster atz= 1.62

Hatch

Muldrew

Cooke

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Observations in the visible wavelengths (BVRi filters) were performed using the EFOSC2 instrument (Buzzoni et al 1984) mounted on the NTT (since April 2008; Snodgrass et al 2008); while near-infrared observations (J, CH 4 filters) were performed using the widefield camera Hawk-I (Pirard et al 2004;Casali et al 2006;Kissler-Patig et al 2008) installed on the UT4/Yepun telescope. We use the medium-width CH 4 filter as a narrow H band (1.52-1.63 μm, hereafter H S ) to measure the J-H S colour as a sensitive test for water ice (see Snodgrass et al 2010, for details).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Characterisation of candidate members of (136108) Haumea’s family

Carry

Snodgrass

Lacerda

et al. 2012

A&A

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Context. From a dynamical analysis of the orbital elements of trans-Neptunian objects (TNOs), , AJ, 134, 2160 reported a list of candidate members of the first collisional family found among this population, associated with (136 108) Haumea (a.k.a. 2003 EL 61 ). Aims. We aim to distinguish the true members of the Haumea collisional family from interlopers. We search for water ice on their surfaces, which is a common characteristic of the known family members. The properties of the confirmed family are used to constrain the formation mechanism of Haumea, its satellites, and its family. Methods. Optical and near-infrared photometry is used to identify water ice. We use in particular the CH 4 filter of the Hawk-I instrument at the European Southern Observatory Very Large Telescope as a short H-band (H S ), the (J − H S ) colour being a sensitive measure of the water ice absorption band at 1.6 μm. Results. Continuing our previous study headed by Snodgrass, we report colours for 8 candidate family members, including nearinfrared colours for 5. We confirm one object as a genuine member of the collisional family (2003 UZ 117 ), and reject 5 others. The lack of infrared data for the two remaining objects prevent any conclusion from being drawn. The total number of rejected members is therefore 17. The 11 confirmed members represent only a third of the 36 candidates. Conclusions. The origin of Haumea's family is likely to be related to an impact event. However, a scenario explaining all the peculiarities of Haumea itself and its family remains elusive.

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“…The near-infrared data presented in this paper were obtained in the context of our large survey of the Carina Nebula (see Preibisch et al 2011c, for more details) with the instrument HAWK-I (see Kissler-Patig et al 2008) at the ESO 8 m Very Large Telescope. HAWK-I is equipped with a mosaic of four Hawaii 2RG 2048 × 2048 pixel detectors with a scale of 0.106 per pixel.…”

Section: Observationsmentioning

confidence: 99%

Detection of a large massive circumstellar disk around a high-mass young stellar object in the Carina Nebula

Preibisch

Ratzka

Gehring

et al. 2011

A&A

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Context. The characterization of circumstellar disks around young stellar objects can provide important information about the process of star formation and the possible formation of planetary systems. Aims. We investigate the spatial structure and the spectral energy distribution of a newly discovered edge-on circumstellar disk around an optically invisible young stellar object that is embedded in a dark cloud in the Carina Nebula. Methods. The disk object was serendipitously discovered in our deep near-IR imaging survey of the Carina Nebula obtained with HAWK-I at the ESO VLT. Whereas the object was detected as an apparently point-like source in earlier infrared observations, only the superb image quality (FWHM ≈ 0.5 ) of the HAWK-I data could reveal, for the first time, the peculiar morphology of the object. It consists of a very red point-like central source that is surrounded by a roughly spherical nebula, which is intersected by a remarkable dark lane through the center. We construct the spectral energy distribution of the object from 1 μm to 870 μm and perform a detailed radiative transfer modeling of the spectral energy distribution and the source morphology. Results. The observed object morphology in the near-IR images clearly suggests a young stellar object that is embedded in an extended, roughly spherical envelope and surrounded by a large circumstellar disk with a diameter of ≈5500 AU that is seen nearly edge-on. The radiative transfer modeling shows that the central object is highly luminous and thus must be a massive young stellar object, most likely in the range 10−15 M . The circumstellar disk has a mass of about 2 M . Conclusions. The disk object in Carina is one of the most massive young stellar objects for which a circumstellar disk has been detected so far. The size and mass of the disk are very large compared to the corresponding values found for most other similar objects. These results support the assumption that 10−15 M stars can form via accretion from a circumstellar disk.

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HAWK-I: the high-acuity wide-field K-band imager for the ESO Very Large Telescope

Cited by 139 publications

References 7 publications

The structure and evolution of a forming galaxy cluster atz= 1.62

The structure and evolution of a forming galaxy cluster atz= 1.62

Characterisation of candidate members of (136108) Haumea’s family

Detection of a large massive circumstellar disk around a high-mass young stellar object in the Carina Nebula

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