Binary star observations with the Hubble Space Telescope fine guidance sensors. II - Bright Hyades

Franz, O. G.; Wasserman, L. H.; Nelan, E.; Lattanzi, M. G.; Bucciarelli, B.; Taff, L. G.

doi:10.1086/116051

Cited by 19 publications

(16 citation statements)

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“…Figure 5 shows the transfer functions of GJ 54AB, LHS 224AB, and the single star HIP 28355, measured along orthogonal axes of FGS1r. These X and Y transfer functions track the visibility of the broadband fringes as the stars are scanned across the Koester's prism (Franz et al 1992). The transfer functions of a single star (left panels of Figure 5) are generally antisymmetric about the zero scan position that denotes alignment between the incoming wavefront and the optical axis.…”

Section: Gj 54ab and Lhs 224abmentioning

confidence: 95%

The Solar Neighborhood. IX.Hubble Space TelescopeDetections of Companions to Five M and L Dwarfs within 10 Parsecs of the Sun

et al. 2004

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We report the detections of low-mass companions to five M and L dwarfs within 10 pc of the Sun using the Hubble Space Telescope (HST) Near-Infrared Camera and Multi-Object Spectrometer (NICMOS). Follow-up observations using the HST Advanced Camera for Surveys (ACS) and Fine Guidance Sensor 1r (FGS1r) confirm our NICMOS discoveries of companions to the L4.5 dwarf GJ 1001B (LHS 102B) and the M5 dwarf LHS 224, respectively. Images obtained with the Astrophysical Research Consortium 3.5 m telescope at Apache Point Observatory verify our discovery of a companion to the M3 dwarf G 239-25. Our NICMOS images confirm the previously suspected duplicity of the M3 dwarfs GJ 54 and GJ 84. The components of GJ 1001BC and LHS 224AB have nearly equal luminosities in all the ACS and/or NICMOS bandpasses in which they were observed. The magnitudes of GJ 54A and B in one FGS1r bandpass and four NICMOS bandpasses differ by 1. GJ 84B and G 239-25B are ∼ 4 magnitudes -2fainter than their M3 companions in the NICMOS bandpasses. We estimate from our NICMOS photometry that GJ 84B and G 239-25B have spectral types M7 and M8, respectively, and masses near the lower limit for sustained hydrogen burning. The apparent separations of GJ 1001BC, GJ 54AB, and LHS 224AB suggest orbital periods less than 5 yr. These binary dwarfs are ideal candidates for continued astrometric monitoring that will quickly yield accurate dynamic masses needed to constrain the mass-luminosity relation for low-mass stars and brown dwarfs.

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Section: Gj 54ab and Lhs 224abmentioning

confidence: 95%

The Solar Neighborhood. IX.Hubble Space TelescopeDetections of Companions to Five M and L Dwarfs within 10 Parsecs of the Sun

et al. 2004

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“…The FGS astrometer offers many observation capabilities (Nelan et al 1998) that have already been used in the past for binary stars (Franz et al 1991(Franz et al , 1992Bernacca et al 1993Bernacca et al , 1995Schneider et al 1998), extended Miras (Lattanzi et al 1994(Lattanzi et al , 1997 and AGN (Hook et al 2000). For such objects the fringe pattern or S -curve changes with respect to that of a point-like source.…”

Section: Effects Of Size and Duplicitymentioning

confidence: 99%

Asteroids observations with the Hubble Space Telescope FGS

Hestroffer¹,

Tanga²,

Cellino³

et al. 2002

A&A

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Abstract. Five main belt asteroids and one Trojan -selected mainly on the basis of their possible binary nature as deduced from light curve morphology -have been observed with the Fine Guidance Sensors (FGS#3 and FGSR#1) of the Hubble Space Telescope (HST). In this first paper we present the selection and observation strategy, data reduction and analysis. A careful analysis of the precision for derived parameters is also given. The HST/FGS proves to be valuable in determining asteroid sizes, shapes and spin axis orientations, and also to identify nearly-contact binary systems.

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“…The FGS is used in TRANS mode by scanning the instantaneous field of view (IFOV) across the star and recording the difference in photometric counts from pairs of photomultiplier tubes in two orthogonal directions (denoted X and Y). The resulting transfer function (TF) measures the interference pattern between detectors, and in the case of a binary star, the observed TF is a convolution of the TF for a single star with two ␦ functions representing the projected separation and magnitude difference of the pair (Franz et al 1992;Lattanzi et al 1992). The binary separations are then measured by fitting the observations with a composite TF formed by co-addition of two shifted and weighted single-star TFs.…”

Section: Hst͞fgs Astrometry and Astrometric Orbitmentioning

confidence: 99%

The O-Type Binary 15 Monocerotis Nears Periastron

Gies¹,

Mason²,

Bagnuolo³

et al. 1997

The Astrophysical Journal

222

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We present new radial velocity measurements for the massive binary 15 Monocerotis which indicate that the system is now very close to periastron (1996.9) in its 24 yr orbit. The velocity separation in the coming year may be large enough to permit an accurate estimate of mass ratio. We also present our first astrometric measurement of 15 Mon made with the Hubble Space Telescope Fine Guidance Sensors (FGS). The FGS transfer functions are consistent with an advanced orbital position close to periastron, and we present preliminary orbital elements for the combined spectroscopic and astrometric orbit.

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Binary star observations with the Hubble Space Telescope fine guidance sensors. II - Bright Hyades

Cited by 19 publications

References 0 publications

The Solar Neighborhood. IX.Hubble Space TelescopeDetections of Companions to Five M and L Dwarfs within 10 Parsecs of the Sun

The Solar Neighborhood. IX.Hubble Space TelescopeDetections of Companions to Five M and L Dwarfs within 10 Parsecs of the Sun

Asteroids observations with the Hubble Space Telescope FGS

The O-Type Binary 15 Monocerotis Nears Periastron

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