Seoul National University 4k×4k Camera (Snucam) for Maidanak Observatory

Im, Myungshin; Ko, Jongwan; Cho, Yun-Seok; Choi, Changsu; Jeon, Yiseul; Lee, In-Duk; Ibrahimov, M.

doi:10.5303/jkas.2010.43.3.075

Cited by 57 publications

(42 citation statements)

References 18 publications

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“…We also observed several regions in IC 1805, for a study of the reddening and massive star content, using the SITe 2000×800 CCD (Maidanak 2k CCD) and standard U BV RI filters of the AZT-22 1.5m telescope at the Maidanak Astronomical Observatory in Uzbekistan. Later, we obtained additional images of the central region of IC 1805 with the Fairchild 486 CCD (SNUCam -Lim et al 2009;Im et al 2010) and U BV I and Hα filters of the AZT-22 telescope. The optical observations are summarized in Table 1.…”

Section: Optical Photometrymentioning

confidence: 99%

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

Sung

Bessell

Chun

et al. 2017

ApJS

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We present deep wide-field optical CCD photometry and mid-infrared Spitzer/IRAC and MIPS 24µm data for about 100,000 stars in the young open cluster IC 1805. The members of IC 1805 were selected from their location in the various color-color and color-magnitude diagrams, and the presence of Hα emission, mid-infrared excess emission, and X-ray emission. The reddening law toward IC 1805 is nearly normal (R V = 3.05 ± 0.06). However, the distance modulus of the cluster is estimated to be 11.9 ± 0.2 mag (d = 2.4 ± 0.2 kpc) from the reddening-free color-magnitude diagrams, which is larger than the distance to the nearby massive star-forming region W3(OH) measured from the radio VLBA astrometry. We also determined the age of IC 1805 (τ M ST O = 3.5 Myr). In addition, we critically compared the age and mass scale from two pre-main-sequence evolution models. The initial mass function with a Salpeter-type slope of Γ = -1.3 ± 0.2 was obtained and the total mass of IC 1805 was estimated to be about 2700 ± 200 M . Finally, we found our distance determination to be statistically consistent with the Tycho-Gaia Astrometric Solution Data Release 1, within the errors. The proper motion of the B-type stars shows an elongated distribution along the Galactic plane, which could be explained by some of the B-type stars being formed in small clouds dispersed by previous episodes of star formation or supernova explosions.

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Section: Optical Photometrymentioning

confidence: 99%

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

Sung

Bessell

Chun

et al. 2017

ApJS

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“…We obtained optical observations with many ground‐based telescopes: the 2‐m Faulkes Telescope North; the 2‐m Liverpool Telescope; the 8.1‐m Gemini ‐North; the 4.2‐m William‐Herschel Telescope (WHT); the 2.5‐m Isaac Newton Telescope (INT); the 2.6‐m Shajn telescope of CrAO; the 1.25‐m AZT‐11 telescope of CrAO; the 1.5‐m Maidanak AZT‐22 telescope with the SNUCAM CCD camera (Im et al 2010); the 1.5‐m AZT‐33IK telescope of Sayan observatory, Mondy; the 6‐m BTA‐6 optical telescope and the 1‐m Zeiss‐1000 telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO‐RAS); the 1‐m LOAO telescope (Lee, Im & Urata 2010) at Mt. Lemmon (Arizona, USA) which is operated by the Korea Astronomy Space Science Institute; 15.5‐cm telescope at Bohyunsan Optical Astronomy Observatory (BOAO) in Korea which is operated by the Korea Astronomy Space Science Institute; the 2‐m Himalayan Chandra Telescope (HCT) and the T40 telescope at the Observatorio de Aras de los Olmos, operated by the Observatori Astronómic de la Universitat de València.…”

Section: Grb 090618mentioning

confidence: 99%

A tale of two GRB-SNe at a common redshift of z=0.54

Cano¹,

Bersier²,

Guidorzi³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present ground-based and Hubble Space Telescope optical observations of the optical transients (OTs) of long-duration Gamma Ray Bursts (GRBs) 060729 and 090618, both at a redshift of z = 0.54. For GRB 060729, bumps are seen in the optical light curves (LCs), and the late-time broad-band spectral energy distributions (SEDs) of the OT resemble those of local Type Ic supernovae (SNe). For GRB 090618, the dense sampling of our optical observations has allowed us to detect well-defined bumps in the optical LCs, as well as a change in colour, that are indicative of light coming from a core-collapse SN. The accompanying SNe for both events are individually compared with SN1998bw, a known GRB supernova, and SN1994I, a typical Type Ic supernova without a known GRB counterpart, and in both cases the brightness and temporal evolution more closely resemble SN1998bw. We also exploit our extensive optical and radio data for GRB 090618, as well as the publicly available Swift-XRT data, and discuss the properties of the afterglow at early times. In the context of a simple jet-like model, the afterglow of GRB 090618 is best explained by the presence of a jet-break at t − t o > 0.5 d. We then compare the rest-frame, peak V-band absolute magnitudes of all of the GRB and X-Ray Flash (XRF)-associated SNe with a large sample of local Type Ibc SNe, concluding that, when host extinction is considered, the peak magnitudes of the GRB/XRF-SNe cannot be distinguished from the peak magnitudes of non-GRB/XRF SNe.

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“…An important upgrade of the telescope occurred in 2006 by installing the SNUCAM camera, which uses a CCD detector with a 0 . 266 pixel −1 scale (Im et al 2010). Although this camera is still working on the MT, we used the FLI MicroLine CCD with a pixel scale of 0 .…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Liverpool-Maidanak monitoring of the Einstein Cross in 2006–2019

Goicoechea

Артамонов

Shalyapin

et al. 2020

A&A

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Quasar microlensing offers a unique opportunity to resolve tiny sources in distant active galactic nuclei and study compact object populations in lensing galaxies. We therefore searched for microlensing-induced variability of the gravitationally lensed quasar QSO 2237+0305 (Einstein Cross) using 4374 optical frames taken with the 2.0 m Liverpool Telescope and the 1.5 m Maidanak Telescope. These gVrRI frames over the 2006–2019 period were homogeneously processed to generate accurate long-term multi-band light curves of the four quasar images A–D. Through difference light curves, we found strong microlensing signatures. We then focused on the analytical modelling of two putative caustic-crossing events in image C, finding compelling evidence that this image experienced a double caustic crossing. Additionally, our overall results indicate that a standard accretion disc accounts reasonably well for the brightness profile of UV continuum emission sources and for the growth in source radius when the emission wavelength increases: Rλ ∝ λα, α = 1.33 ± 0.09. However, we caution that numerical microlensing simulations are required before firm conclusions can be reached on the UV emission scenario because the VRI-band monitoring during the first caustic crossing and one of our two α indicators lead to a few good solutions with α ≈ 1.

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Seoul National University 4k×4k Camera (Snucam) for Maidanak Observatory

Cited by 57 publications

References 18 publications

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

A tale of two GRB-SNe at a common redshift of z=0.54

Liverpool-Maidanak monitoring of the Einstein Cross in 2006–2019

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Seoul National University 4k×4k Camera (Snucam) for Maidanak Observatory

Cited by 57 publications

References 18 publications

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* †

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* †

A tale of two GRB-SNe at a common redshift of z=0.54

Liverpool-Maidanak monitoring of the Einstein Cross in 2006–2019

Contact Info

Product

Resources

About

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†

An Optical and Infrared Photometric Study of the Young Open Cluster IC 1805 in the Giant H ii Region W4* ^†