Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.adass.org/adass/proceedings/adass96/reprints/chans2.pdf Дата изменения: Wed Jan 14 23:14:54 1998 Дата индексирования: Tue Oct 2 11:42:04 2012 Кодировка: Поисковые слова: molecular cloud

Astronomical Data Analysis Software and Systems VI ASP Conference Series, Vol. 125, 1997 Gareth Hunt and H. E. Payne, eds.

Near-IR Imaging of Star-forming Regions with IRAF
S. J. Chan and A. Mampaso Instituto de Astrofґ a de Canarias, C/Via Lґ tea s/n, E-38200 La isic ac Laguna, Tenerife, Spain Abstract. We rep ort on our ongoing pro ject "Infrared Study of H ii Regions Associated with Small Clouds." Several tasks are b eing develop ed under the IRAF environment for efficiently reducing and analyzing the near-infrared data obtained from the Teide observatory with the IAC infrared camera (IAC-IRCAM).

1.

Introduction

Several galactic H ii regions associated with small molecular clouds were observed with the IR-Camera on the 1.5 m CST (Carlos Sґ chez Telescop e) of the Teide an Observatory in Octob er 1996. These IR data, combined with optical imaging (which will b e obtained from the IAC-80 telescop e), IRAS survey maps, and existing CO observations of the associated clouds, will allow us to undertake a detailed investigation of the gas-to-dust mass ratio, initial mass function and the star-formation efficiency in these complexes. Studies of the emb edded clusters also allow us to derive the luminosity function and thus, using an appropriate mass-luminosity relation, to determine the stellar mass sp ectrum. The near-IR imaging study will allow us to search systematically for exciting sources and the low-mass stars associated with the nebulФ. Some data were obtained during the test run of the IAC-IRCAM on February 1996. We are using these data to test our new IRCAM package, develop ed under the IRAF environment. 2. 2.1. IRCAM Package IAC-IRCAM 3 array and has a plate seven filters covering the s limiting magnitudes for 16 mag at K.

The IAC-IRCAM is based on a 256в256 NICMOS scale of 0.4 /pixel. Currently, the camera contains wavelength range from 1.2 µm to 2.32 µm. The 3 60 p oint sources were 18.8 mag at J, 18.5 mag at H, and 2.2.

Preliminary Tasks in the IRCAM package

At the time of writing this pap er, eighteen preliminary tasks have b een written. A common characteristic of these tasks is ease in handling the b ookkeeping of data reduction/analysis history. The tasks are as follows: · APCOR: estimate the ap erture correction, 93

© Copyright 1997 Astronomical Society of the Pacific. All rights reserved.


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Chan and Mampaso

Figure 1. Part of the S269 field: left--b efore MDRIPNEW processing; right--after MDRIPNEW processing. · CHECKPSF: check the PSF (Point Spread Function) model, · DUMPMARK: mark and lab el ob jects on the displayed frame, · EXAMPSFGP: examine the PSF model, · FINMISS: find missing stars not found with DAOFIND, · FINSHIFT: find the image shifts with resp ect to the reference image, · FINFIT: fit all the stars, including the missing stars, with the final PSF model, · FIRSTPSF: obtain the first iteration of a PSF model, · MARK3FR: display all the frames and mark the stars, · MATCHMARK: find the stars which match all the frames, · MATCHPHOT: obtain the photometry from the match frame and produce a final list, · MDRIPNEW: reduce the "drip" noise produced by the IAC-IRCAM (see Figure 1), · NITERPSF: obtain the nth iteration PSF model, · PARFIND: find the critical parameters from the frames, · SELBRIGHT: select well isolated bright stars, · SELPST1: select first iteration PSF candidates, and · SUBMARK: subtract the neighb ours and their friends from the PSF stars and display the subtracted image.


Near-IR Imaging of Star-forming Regions with IRAF 2.3. Future Development of IRCAM

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Future tasks include: · writing help pages for the tasks, · using new IRCAM data to test every detail of the package, · write more tasks based on IMAGES, IMMATCH, and DIMSUM packages (brand-new tasks will b e written if necessary), · combine several small tasks into a single task, and · if satisfied with the p erformance of this package, release it to the public. Acknowledgments. S. J. Chan thanks the Program Organizing Committee for the Sixth Annual Astronomical Data Analysis Software and System Conference for offering her full financial supp ort to attend the Conference.