&lt;title&gt;GMOS: the GEMINI Multiple Object Spectrographs&lt;/title&gt;

Davies, Roger L.; Allington‐Smith, J. R.; Bettess, P.; Chadwick, Edmund; Content, Robert; Dodsworth, George N.; Haynes, Roger; Lee, David; Lewis, Ian; Webster, John R. P.; Ettedgui-Atad, Eli; Beard, S. M.; Ellis, Maureen A.; Hastings, Peter; Williams, P.; Bond, Tim; Crampton, D.; Davidge, T. J.; Fletcher, J. M.; Leckie, Brian; Morbey, C. L.; Murowinski, Richard; Roberts, Scott; Saddlemyer, Leslie; Sebesta, Jerry; Stilburn, James R.; Szeto, Kei

doi:10.1117/12.268996

Cited by 49 publications

(15 citation statements)

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“…The Gemini-North instrument used for optical imaging was GMOS (Davies et al 1997;Hook et al 2004). Data were acquired on UT 2011 February 2.…”

Section: Optical Imagingmentioning

confidence: 99%

The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

Aspin

2011

The Astronomical Journal

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We present optical and near-IR observations of the young eruptive variable star V1647 Orionis which illuminates McNeil's Nebula. In late 2003, V1647 Ori was observed to brighten by around 5 mag to r = 17.7. In early 2006 the star faded back to its quiescent brightness of r ∼ 23, however in mid-2008 it brightened yet again by ∼5 mag. Our new observations, taken in early 2011, show V1647 Ori to be in an elevated photometric state with an optical brightness similar to the value found at the start of the 2003 and 2008 outbursts. Optical images taken between 2008 and 2011 suggest that the star has remained in outburst from mid-2008 to the present. Hα and the far-red Ca ii triplet lines remain in emission with Hα possessing a significant P Cygni profile. A self-consistent study of the accretion luminosity and rate using data taken in 2004, 2007, 2008, and 2011 indicates that when bright, V1647 Ori has values of 16 ± 2 L and (4 ± 2) × 10 −6 M yr −1 , respectively. We support the premise that the accretion luminosity and rate both declined by a factor of 2-3 during the 5 mag fading in 2007. However, a significant part of the fading was due to either variable extinction or dust reformation. We discuss these new observations in relation to previous published data and the classification schemes for young eruptive variables.

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“…The Gemini-North instrument used for optical imaging was GMOS (Davies et al 1997;Hook et al 2004). Data were acquired on UT 2011 February 2.…”

Section: Optical Imagingmentioning

confidence: 99%

The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

Aspin

2011

The Astronomical Journal

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“…All but one data set presented below were acquired using the "Frederick C. Gillett" Gemini North telescope located on Mauna Kea, Hawaii using the facility optical imager and spectrograph, GMOS-N (Davies et al 1997;Hook et al 2004). The imaging observations used standard GMOS-N g , r , i , and z filters which were designed to be as close as possible in characteristics to the Sloan Digital Sky Survey (SDSS) filters (Fukugita et al 1996).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Aspin

Reipurth

2009

The Astronomical Journal

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We present results from an optical imaging and spectroscopic monitoring campaign on the young, low-mass eruptive variable star V1647 Orionis. The star and associated nebulosity (McNeil's Nebula) were observed over the period 2004 February to 2006 February with observations commencing a few months after the original outburst event occurred. Using the Gemini North telescope, we obtained multiband optical imaging photometry and medium-resolution long-slit spectroscopy of V1647 Ori on an approximately monthly interval. During this period, V1647 Ori remained at, or close to, peak brightness and then faded by 5 mag to close to its pre-outburst brightness. This implies an outburst timescale of around 27 months. Spectral features seen in both emission and absorption varied considerably during the monitoring period. For example, the Hα line changed significantly in both intensity and profile. We present and discuss the observed photometric and spectroscopic changes and consider how this eruptive event relates to the early formative stages of low-mass stars.

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“…Here the object selection is achieved by a drilled or cut slit pattern in a mask plate. [4][5][6] For every observation a new plate with a new pattern has to be prepared. Other systems for ground based MOS observations are based on fibers.…”

Section: Introductionmentioning

confidence: 99%

Integral field and multi-object spectrometry with MEMS

Wuttig¹,

Riesenberg²,

Nitzsche³

2002

SPIE Proceedings

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Multi object spectrometers measure spectra of multiple objects simultaneously. Besides others, e.g. fiber positioning systems, there is a class of multi object spectrometers which is based on a dispersing imaging optics in connection with a slit masks. Two considered approaches for reconfigurable slit masks are two-dimensional MEMS arrays, such as micro mirror or micro shutter arrays, and slit positioning devices. After an introduction to multi object spectrometry with dispersing imaging optics we calculate the effective multiplex capabilities of multi object spectrometers based on 2D MEMS and on slit positioning devices for randomly distributed objects. The observation efficiency of multi object spectrometers based on 2D MEMS is compared to integral field spectrometers and to multi object spectrometers based on slit positioning devices. We find that for typical applications the efficiency of the slit positioning approach is nearly as good as the efficiency of the 2D MEMS approach. This makes slit positioning systems a serious alternative solution to 2D MEMS devices as long as they are easier to get.

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<title>GMOS: the GEMINI Multiple Object Spectrographs</title>

Cited by 49 publications

References 0 publications

The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Integral field and multi-object spectrometry with MEMS

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