Omega Prime: the wide-field near-infrared camera for the 3.5-m telescope of the Calar Alto Observatory

Bizenberger, Peter; McCaughrean, M. J.; Birk, Christoph; Thompson, D. J.; Storz, Clemens

doi:10.1117/12.317219

Cited by 37 publications

(32 citation statements)

References 3 publications

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“…A deep broad-band K (1.92-2.29 µm) survey of the Lockman Hole region was carried out with the Omega-Prime camera (Bizenberger et al 1998) at the Calar Alto 3.5 m telescope in 1997 and 1998. This survey covers approximately half the Lockman Hole field.…”

Section: Optical-to-near-ir Coloursmentioning

confidence: 99%

XMM-Newton observation of the Lockman Hole

Mainieri

Bergeron

Hasinger

et al. 2002

A&A

202

295

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Abstract. We present the results of the X-ray spectral analysis of the first deep X-ray survey with the XMM-Newton observatory during Performance Verification. The X-ray data of the Lockman Hole field and the derived cumulative source counts were reported by Hasinger et al. (2001). We restrict the analysis to the sample of 98 sources with more than 70 net counts (flux limit in the [0.5-7] keV band of 1.6 × 10 −15 erg cm −2 s −1 ) of which 61 have redshift identification. We find no correlation between the spectral index Γ and the intrinsic absorption column density N H and, for both the Type-1 and Type-2 AGN populations, we obtain Γ 2. The progressive hardening of the mean X-ray source spectrum with decreasing flux is essentially due to an increase in intrinsic absorption. The marked separation between the two AGN populations in several diagnostics diagrams, involving X-ray colour, X-ray flux, optical/near IR colour and optical brightness, is also a consequence of different absorption column densities and enables the classification of optically faint obscured AGN. The Type-2 and obscured AGN have weaker soft X-ray and optical fluxes and redder R − K colours. They follow the evolutionary tracks of their host galaxies in a colorredshift diagram. About 27% of the subsample with R − K colour are EROs (R − K ≥ 5) and most of these 18 X-ray selected EROs contain an obscured AGN as revealed by their high X-ray-to-optical/near IR flux ratios. There are six sources in our sample with L X [0.5−10] > 10 44 erg s −1 and log(N H ) > 10 22 cm −2 : which are likely Type-2 QSOs and we thus derive a density of ∼69 objects of this class per square degree.

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Section: Optical-to-near-ir Coloursmentioning

confidence: 99%

XMM-Newton observation of the Lockman Hole

Mainieri

Bergeron

Hasinger

et al. 2002

A&A

202

295

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“…Observations were done using Full MPIA double correlated read mode (see Bizenberger et al 1998, for full description), which has a minimum detector integration time (DIT) of 1.677 s. By using this method each "individual frame" was constructed from 47 co-added DITs resulting in about 79 s of integration. In this way, 9 frames were taken with a standard 5-point jittering.…”

Section: Imagingmentioning

confidence: 99%

“…For the NIR images we first used the Omega Prime (Bizenberger et al 1998) camera at the Calar Alto 3.5 m telescope, Spain (see Table 1). Observations were done using Full MPIA double correlated read mode (see Bizenberger et al 1998, for full description), which has a minimum detector integration time (DIT) of 1.677 s. By using this method each "individual frame" was constructed from 47 co-added DITs resulting in about 79 s of integration.…”

Section: Imagingmentioning

confidence: 99%

An outbursting protostar of the FU Orionis type in the Cygnus OB7 molecular cloud

Movsessian¹,

Khanzadyan

Aspin³

et al. 2006

A&A

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Context. To follow the early evolution of stars we need to understand how young stars accrete and eject mass. It is generally assumed that the FU Orionis phenomenon is related to the variations in the disk accretion, but many questions remain still open, in particular because of the rarity of FU Ori type stars. Aims. We explore here the characteristics of the outburst and of the environment of one new object, discovered recently in the active star formation region containing RNO 127, within the Cygnus OB7 dark cloud complex. Methods. We present an extensive optical and near-infrared study of a new candidate of FU Orionis object, including its direct imaging, spectroscopy and scanning Fabry-Pérot interferometry. Results. The source, associated with the variable reflection nebula, underwent prodigious outburst. The "Braid" nebula, which appeared in 2000, as is indicated by its name, consists of two intertwined features, illuminated by the outburst. Subsequent NIR observations revealed the bright source, which was not visible on 2MASS images, and its estimated brightening was more than 4 mag. Optical and infrared spectral data show features, which are necessary for the system to be referred to as a FUor object. The bipolar optical flow directed by the axis of nebula also was found. Various estimates give the November/December 1999 as the most probable date for the eruption.

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“…The Calar Alto observations were carried out during three first half nights of August 10−13, 2003. Omega Prime (Bizenberger et al 1998) is equipped with a Rockwell 1024 × 1024 pixel HAWAII array detector and provides a fixed pixel scale of 0.4 arcsec/pixel. The total field of view covered in one integration is 6.…”

Section: Observing Strategymentioning

confidence: 99%

An unbiased search for the signatures of protostars in the ρ Ophiuchi A molecular cloud

Khanzadyan¹,

Gredel²,

Smith³

et al. 2004

A&A

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Abstract. We present an unbiased search for molecular hydrogen emission in the L1688 cloud within the ρ Ophiuchi molecular cloud complex. Our near-infrared survey covers a connected region of extent 35 × 35 . We detect several new H 2 flows but the total number of detected outflows is low and is consistent with the paucity of Class 0 and Class 1 sources in the molecular cloud. From the spatial distribution, their collimation and the individual shapes of the bow shocks, we suggest possible candidates for the outflow sources. Most of the candidate driving sources are deeply embedded in dense cores of the molecular cloud. A very young outflow arises from the newly discovered Class 0 source MMS 126. Two major outflows in the NE-SW direction arise from the YLW 15 and YLW 16 Class I sources. Three additional outflows, which both extend over several arcminutes, arise from the Class I sources YLW 31 and YLW 52. Flow directions are generally NE-SW, perpendicular to the elongation directions of the cloud filaments. The apparent extents of molecular flows are related to either the widths of cloud filaments or to the separation between filaments. The estimated jet power needed to continuously drive and excite the detected portions of the shocked H 2 outflows lies in the range 0.02−0.2 L . Given the critical dependence on the environment, however, the total sizes and powers of the outflows may be considerably larger.

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Omega Prime: the wide-field near-infrared camera for the 3.5-m telescope of the Calar Alto Observatory

Cited by 37 publications

References 3 publications

XMM-Newton observation of the Lockman Hole

XMM-Newton observation of the Lockman Hole

An outbursting protostar of the FU Orionis type in the Cygnus OB7 molecular cloud

An unbiased search for the signatures of protostars in the ρ Ophiuchi A molecular cloud

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