The FAST Spectrograph for the Tillinghast Telescope

Fabricant, Daniel G.; Cheimets, Peter; Caldwell, Nelson; Geary, John C.

doi:10.1086/316111

Cited by 282 publications

(257 citation statements)

References 2 publications

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“…Spectra of the OT associated with GRB 030329 were obtained over many nights with the 6.5 m Multiple Mirror Telescope (MMT), the 1.5 m Tillinghast telescope at the Fred Lawrence Whipple Observatory (FLWO), and the Magellan 6.5 m Clay telescope. The spectrographs used were the Blue Channel (Schmidt et al 1989) at the MMT, FAST (Fabricant et al 1998) at the FLWO 60 inch (1.5 m) telescope, and LDSS2 12 at Magellan. The observations were reduced in the standard manner with IRAF 13 and our own routines.…”

Section: Observationsmentioning

confidence: 99%

Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329

Stanek

Matheson

Garnavich

et al. 2003

ApJ

1,178

1,052

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We present early observations of the afterglow of GRB 030329 and the spectroscopic discovery of its associated supernova SN 2003dh. We obtained spectra of the afterglow of GRB 030329 each night from March 30.12 (0.6 days after the burst) to April 8.13 (UT) (9.6 days after the burst). The spectra cover a wavelength range of 350-850 nm. The early spectra consist of a power-law continuum ( ) with narrow emission lines orig-Ϫ0.9

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Section: Observationsmentioning

confidence: 99%

Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329

Stanek

Matheson

Garnavich

et al. 2003

ApJ

1,178

1,052

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“…The instrumental set-up for the 1.3 m telescope of the Skinakas Observatory was a 2000 × 800 ISA SITe CCD and a 1302 l mm −1 grating, giving a nominal dispersion of ∼1.04 Å/pixel, while for the 1.5-m telescope at Mt. Hopkins (Arizona), the FAST-II spectrograph (Fabricant et al 1998) plus FAST3 CCD, a backsideilluminated 2688 × 512 UA STA520A chip with 15 µm pixels and a 1200 l mm −1 grating (0.38 Å/pixel). Occasionally, a 2400 l mm −1 and a 600 l mm −1 grating was used in Skinakas and Mt.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Long-term optical variability of high-mass X-ray binaries

Reig

Nersesian

Zezas

et al. 2016

A&A

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Context. High-mass X-ray binaries are bright X-ray sources. The high-energy emission is caused by the accretion of matter from the massive companion onto a neutron star. The accreting material comes from either the strong stellar wind in binaries with supergiant companions or the cirscumstellar disk in Be/X-ray binaries. In either case, the Hα line stands out as the main source of information about the state of the accreting material. Aims. We present the results of our monitoring program to study the long-term variability of the Hα line in high-mass X-ray binaries. Our aim is to characterise the optical variability timescales and study the interaction between the neutron star and the accreting material. Methods. We fitted the Hα line with Gaussian profiles and obtained the line parameters and equivalent width. The peak separation in split profiles was used to determine the disk velocity law and estimate the disk radius. The relative intensity of the two peaks (V/R ratio) allowed us to investigate the distribution of gas particles in the disk. The equivalent width was used to characterise the degree of variability of the systems. We also studied the variability of the Hα line in correlation with the X-ray activity. Results. Our results can be summarised as follows: i) we find that Be/X-ray binaries with narrow orbits are more variable than systems with long orbital periods; ii) we show that a Keplerian distribution of gas particles provides a good description of the disks in Be/X-ray binaries, as it does in classical Be stars; iii) a decrease in the Hα equivalent width is generally observed after major X-ray outbursts; iv) we confirm that the Hα equivalent width correlates with disk radius; v) while systems with supergiant companions display multistructured profiles, most of the Be/X-ray binaries show, at some epoch, double-peak asymmetric profiles, which indicates that density inhomogeneities is a common property in the disk of Be/X-ray binaries; vi) the profile variability (V/R ratio) timescales are shorter and the Hα equivalent widths are smaller in Be/X-ray binaries than in isolated Be stars; and vii) we provide new evidence that the disk in Be/X-ray binaries is, on average, denser than in classical Be stars. Conclusions. We carried out the most complete optical spectroscopic study of the global properties of high-mass X-ray binaries with the analysis of more than 1100 spectra from 20 sources. Our results provide further evidence for the truncation of the disk in Be/X-ray binaries. We conclude that the interaction between the compact object and the Be-type star works in two directions: the massive companion provides the source of matter for accretion, affecting the surroundings of the compact object, and the continuous revolution of the neutron star around the optical counterpart also produces the truncation of the Be star's equatorial disk.

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“…The spectra were obtained on the 1.5 m telescope of the Whipple Observatory with the FAST spectrograph (Fabricant et al 1998), equipped with the Loral 512 ; 2688 CCD. The spectrograph was set up in the standard configuration used for ''FAST COMBO'' projects, a 300 groove mm À1 grating and a 3 00 wide slit.…”

Section: Spectroscopymentioning

confidence: 99%

The Mass Accretion Rates of Intermediate-Mass T Tauri Stars

Calvet¹,

Muzerolle²,

Briceño³

et al. 2004

409

537

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We present Hubble Space Telescope ultraviolet spectra and supporting ground-based data for a sample of nine intermediate-mass T Tauri stars (IMTTSs; 1.5-4 M ). The targets belong to three star-forming regions: T Tau, SU Aur, and RY Tau in the Taurus clouds; EZ Ori, P2441, and V1044 Ori in the Ori OB1c association surrounding the Orion Nebula cluster; and CO Ori, GW Ori, and GX Ori in the ring around k Ori. The supporting groundbased observations include nearly simultaneous UBV(R I ) C photometry, 6 8 resolution spectra covering the range 3900-7000 8, optical echelle observations in the range 5800-8600 8, and K-band near-infrared spectra. We use these data to determine improved spectral types and reddening corrections and to obtain physical parameters of the targets. We find that an extinction law with a weak 2175 8 feature but high values of A UV =A V is required to explain the simultaneous optical-UV data; the reddening laws for two B-type stars located behind the Taurus clouds, HD 29647 and HD 283809, meet these properties. We argue that reddening laws with these characteristics may well be representative of cold, dense molecular clouds. Spectral energy distributions and emission-line profiles of the IMTTSs are consistent with expectations from magnetospheric accretion models. We compare our simultaneous optical-UV data with predictions from accretion shock models to get accretion luminosities and mass accretion rates (Ṁ ) for the targets. We find that the average mass accretion rate for IMTTSs is $3 ; 10 À8 M yr À1 , a factor of $5 higher than that for their low-mass counterparts. The new data extend the correlation betweenṀ and stellar mass to the intermediate-mass range. Since the IMTTSs are evolutionary descendants of the Herbig Ae/ Be stars, our results put limits to the mass accretion rates of their disks. We present luminosities of the UV lines of highly ionized metals and show that they are well above the saturation limit for magnetically active cool stars but correlate strongly with accretion luminosity, indicating that they are powered by accretion, in agreement with previous claims but using a sample in which reddening and accretion luminosities have been determined self-consistently. Finally, we find that the relation between accretion luminosity and Br luminosity found for low-mass T Tauri stars extends to the intermediate-mass regime.

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The FAST Spectrograph for the Tillinghast Telescope

Cited by 282 publications

References 2 publications

Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329

Spectroscopic Discovery of the Supernova 2003dh Associated with GRB 030329

Long-term optical variability of high-mass X-ray binaries

The Mass Accretion Rates of Intermediate-Mass T Tauri Stars

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