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The opposition effect of the asteroid 4 Vesta
Hasegawa, Sunao,Miyasaka, Seidai,Tokimasa, Noritaka,Sogame, Akito,Ibrahimov, Mansur A.,Yoshida, Fumi,Ozaki, Shinobu,Abe, Masanao,Ishiguro, Masateru,Kuroda, Daisuke Oxford University Press 2014 Publications of the Astronomical Society of Japan Vol.66 No.5
THE INITIAL MASS FUNCTION AND YOUNG BROWN DWARF CANDIDATES IN NGC 2264. III. PHOTOMETRIC DATA
Sung, Hwankyung,Bessell, Michael S.,Chun, Moo-Young,Karimov, Rivkat,Ibrahimov, Mansur American Institute of Physics 2008 The Astronomical journal Vol.135 No.2
<P>We have performed deep wide-field CCD photometry of the young open cluster NGC 2264 to study the extent of star-forming regions (SFRs) and the shape of the initial mass function. In this paper, we present VRI and Hα photometry for more than 67,000 stars. From the spatial distribution of the selected Hα emission stars, we identify two active SFRs and a less active halo region surrounding these two SFRs. There are several Hα emission stars in the field region outside the halo region, and these may be newly formed stars in the Mon OB1 association surrounding the cluster. The locus of pre-main-sequence (PMS) stars in the I<SUB>C</SUB> versus V − I<SUB>C</SUB> diagram is revised from the distribution of Hα and X-ray emission stars in the diagram. The mean reddening of late-type PMS stars is estimated to be E(B − V) <img entity='thkap' SRC='http://ej.iop.org/icons/Entities/ap.gif' ALT='≈' ALIGN='ABSMIDDLE' /> 0.2 mag using the distribution of X-ray emission stars in the 2MASS color-color diagram. We can confirm that the Hα emission stars below the PMS locus (so-called BMS stars) are bona-fide members of NGC 2264 from their spatial distribution as well as from their near-IR excess in the 2MASS color-color diagram. In addition, four objects around IRS-2 detected with the Spitzer IRAC are also classified as BMS stars.</P>
A Y-BAND LOOK OF THE SKY WITH 1-M CLASS TELESCOPES
Choi, Chang-Su,Im, Myung-Shin,Jeon, Yi-Seul,Ibrahimov, Mansur The Korean Astronomical Society 2012 Journal of The Korean Astronomical Society Vol.45 No.1
Y-band is a broad passband that is centered at ~1 ${\mu}m$. It is becoming a new, popular window for extragalactic study especially for observations of red objects thanks to recent CCD technology developments. In order to better understand the general characteristics of objects in Y-band, and to investigate the promise of Y-band observations with small telescopes, we carried out imaging observations of several extragalactic fields, brown dwarfs, and high redshift quasars with Y-band filter at the Mt. Lemmon Optical Astronomy Observatory and the Maidanak observatory. From our observations, we constrain the bright end of the galaxy and the stellar number counts in Y-band. We also test the usefulness of high redshift quasar (z >6) selection via i - z - Y color-color diagram, to demonstrate that the i - z - Y color-color diagram is effective for the selection of high redshift quasars even with a conventional optical CCD camera installed at a 1-m class telescope.
SEOUL NATIONAL UNIVERSITY 4K×4K CAMERA (SNUCAM) FOR MAIDANAK OBSERVATORY
Im, Myung-Shin,Ko, Jong-Wan,Cho, Yun-Seok,Choi, Chang-Su,Jeon, Yi-Seul,Lee, In-Duk,Ibrahimov, Mansur The Korean Astronomical Society 2010 Journal of The Korean Astronomical Society Vol.43 No.3
We present the characteristics of the Seoul National University 4k Camera (SNUCAM) and report its performance on the 1.5m telescope at the Maidanak observatory in Uzbekistan. SNUCAM is a CCD camera with a pixel scale of 0.266" in $4096{\times}4096$ format, covering $18.1'{\times}18.1'$ field of view on the 1.5m. The camera is currently equipped with Bessell UBVRI, $H{\alpha}$, SDSS ugriz, and Y-band filters, allowing us to carry out a variety of scientific programs ranging from exoplanet studies to survey of quasars at high redshift. We examine properties of SNUCAM such as the bias level and its temporal variation, the dark current, the readout noise, the gain, the linearity, the fringe patterns, the amplifier bias, and the bad pixels. From our observations, we also constructed the master fringe frames in I-, z-, and Y-band. We outline some of the current scientific programs being carried out with SNUCAM, and demonstrate that SNUCAM on the 1.5m can deliver excellent images that reach to the $5-{\sigma}$ detection limits of R~25.5 mag and z~22.7 mag in 1 hour total integration.