A maximum correlation method for image construction of IRAS survey data

Aumann, Hartmut H.; Fowler, J. W.; Melnyk, Michael

doi:10.1086/115448

Cited by 156 publications

(135 citation statements)

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“…3 HiRes uses the Maximum Correlation Method (MCM, Aumann et al 1990) to produce images with better than the nominal resolution of the IRAS data. 4 http://www.jach.hawaii.edu/UKIRT/MHCat/ (Davis et al 2010).…”

Section: Resultsmentioning

confidence: 99%

A wide-field near-infrared H₂2.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

Khanzadyan

Davis

Aspin

et al. 2012

A&A

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Context. Outflows and jets are the first signposts of ongoing star formation processes in any molecular cloud, yet their study in optical bands provides limited results due to the large extinction present. Near-infrared unbiased wide-field observations in the H 2 1−0 S(1) line at 2.122 µm alleviates the problem, enabling us to detect more outflows and trace them closer to their driving sources. Aims. As part of a large-scale multi-waveband study of ongoing star formation in the Braid Nebula star formation region, we focus on a one square degree region that includes Lynds Dark Nebula 1003 and 1004. Our goal is to find all of the near-infrared outflows, uncover their driving sources and estimate their evolutionary phase. Methods. We use near-infrared wide-field observations obtained with WFCAM on UKIRT, in conjunction with previously-published optical and archival MM data, to search for outflows and identify their driving sources; we subsequently use colour−colour analysis to determine the evolutionary phase of each source. Results. Within a one square degree field we have identified 37 complex MHOs, most of which are new. After combining our findings with other wide-field, multi-waveband observations of the same region we were able to discern 28 outflows and at least 18 protostars. Our analysis suggests that these protostars are younger and/or more energetic than those of the Taurus-Auriga region. The outflow data enable us to suggest connection between outflow ejection and repetitive FU Ori outburst events. We also find that star formation progresses from W to E across the investigated region.

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Section: Resultsmentioning

confidence: 99%

A wide-field near-infrared H₂2.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

Khanzadyan

Davis

Aspin

et al. 2012

A&A

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“…Then all the good-quality data were integrated into a single sky map at each of the IPP blue (B IPP ) and red (R IPP ) bands, using a similar algorithm to 1st iteration of the "maximum correlation method" (Aumann et al 1990). The final maps have the angular resolution of ∼ 0 • .7.…”

Section: Observations and Reductionsmentioning

confidence: 99%

Cosmic Optical Background: the view from Pioneer 10/11

et al. 2011

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Abstract. We present the new constraints on the cosmic optical background (COB) obtained from an analysis of the Pioneer 10/11 Imaging Photopolarimeter (IPP) data. After careful examination of data quality, the usable measurements free from the zodiacal light are integrated into sky maps at the blue (∼0.44 µm) and red (∼0.64 µm) bands. Accurate starlight subtraction is achieved by referring to all-sky star catalogs and a Galactic stellar population synthesis model down to 32.0 mag. We find that the residual light is separated into two components: one component shows a clear correlation with thermal 100 µm brightness, while another betrays a constant level in the lowest 100 µm brightness region. Presence of the second component is significant after all the uncertainties and possible residual light in the Galaxy are taken into account, thus it most likely has the extragalactic origin (i.e., the COB). The derived COB brightness is (1.8 ± 0.9) × 10 −9 and (1.2 ± 0.9) × 10 −9 erg s −1 cm −2 sr −1Å−1 at the blue and red band, respectively, or 7.9 ± 4.0 and 7.7 ± 5.8 nW m −2 sr −1 . Based on a comparison with the integrated brightness of galaxies, we conclude that the bulk of the COB is comprised of normal galaxies which have already been resolved by the current deepest observations. There seems to be little room for contributions of other populations including "first stars" at these wavelengths. On the other hand, the first component of the IPP residual light represents the diffuse Galactic light (DGL)-scattered starlight by the interstellar dust. We derive the mean DGL-to-100 µm brightness ratios of 2.1 × 10 −3 and 4.6 × 10 −3 at the two bands, which are roughly consistent with the previous observations toward denser dust regions. Extended red emission in the diffuse interstellar medium is also confirmed.

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“…A Gaussian approximation of the PSF is given with the HiRes maps and is defined by two spatially dependent FWHMs and a rotation angle. For more information on HiRes, please refer to Aumann et al (1990) and Bontekoe et al (1994). Since we are searching for the properties of extended structures, the HiRes IRAS maps were brought to the DC-calibration (Wheelock et al 1994).…”

Section: Iras Hires Datamentioning

confidence: 99%

Multi-wavelength analysis of the dust emission in the Small Magellanic Cloud

Bot

Boulanger

Lagache

et al. 2004

A&A

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Abstract.We present an analysis of dust grain emission in the diffuse interstellar medium of the Small Magellanic Cloud (SMC). This study is motivated by the availability of 170 µm ISOPHOT data covering a large part of the SMC, with a resolution making it possible to disentangle the diffuse medium from the star forming regions. After data reduction and subtraction of Galactic foreground emission, we used the ISOPHOT data together with HiRes IRAS data and ATCA/Parkes combined H  column density maps to determine dust properties for the diffuse medium. We found a far infrared emissivity per hydrogen atom 30 times lower than the Solar neighborhood value. The modeling of the spectral energy distribution of the dust, taking into account the enhanced interstellar radiation field, gives a similar conclusion for the smallest grains (PAHs and very small grains) emitting at shorter wavelength. Assuming Galactic dust composition in the SMC, this result implies a difference in the gas-to-dust ratio (GDR) 3 times larger than the difference in metallicity. This low depletion of heavy elements in dust could be specific of the diffuse ISM and not apply to all the SMC dust if it results from efficient destruction of dust by supernovae explosions.

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A maximum correlation method for image construction of IRAS survey data

Cited by 156 publications

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A wide-field near-infrared H₂2.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

A wide-field near-infrared H₂2.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

Cosmic Optical Background: the view from Pioneer 10/11

Multi-wavelength analysis of the dust emission in the Small Magellanic Cloud

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A maximum correlation method for image construction of IRAS survey data

Cited by 156 publications

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A wide-field near-infrared H22.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

A wide-field near-infrared H22.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

Cosmic Optical Background: the view from Pioneer 10/11

Multi-wavelength analysis of the dust emission in the Small Magellanic Cloud

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Product

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A wide-field near-infrared H₂2.122μm line survey of the Braid Nebula star formation region in Cygnus OB7

A wide-field near-infrared H₂2.122μm line survey of the Braid Nebula star formation region in Cygnus OB7