John S. Tanner Responds

Tanner, John S.

doi:10.2307/376816

Cited by 7 publications

(13 citation statements)

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“…The relative positions of the target and PSF star were estimated using the Poisson spot present in the middle of the coronagraphic spot. As with previous studies (Metchev et al 2004;Tanner et al 2007) we are able to 5 Since the original SIM Lite Palomar survey started in 2004 was meant as a snap-shot program intended to look for close, stellar binaries, a subset of the coronagraphic observations were performed with a neutral density filter which reduced the effective integration times by a factor of 100. In most cases, those stars were reobserved without the neutral density filter to bring the effective integration times up to the level of the rest of the survey targets.…”

Section: Data Reduction and Analysismentioning

confidence: 98%

“…register the star positions to 0.7 pixels using the centroid position of the spot (Tanner et al 2007). The scaling for the PSF is the multiplicative factor which minimizes the residuals remaining after the subtraction.…”

Section: Data Reduction and Analysismentioning

confidence: 99%

“…These programs include radial velocity studies of the reference stars utilized in the narrow-angle observations, accurate spectral type determinations through optical spectroscopy, and photometry studies of the stars in the young star planet search program. Some of these programs have resulted in planet detections themselves (Niedzielski et al 2007) or data that can be applied to upcoming planet surveys (Tanner et al 2007). Here, we present the results of a companion survey of stars included in both of the terrestrial planet SIM Lite surveys.…”

Section: Introductionmentioning

confidence: 99%

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A High-Contrast Imaging Survey ofSIM LitePlanet Search Targets

Tanner¹,

Gelino²,

Law³

2010

PUBL ASTRON SOC PAC

237

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With the development of extreme high contrast ground-based adaptive optics instruments and space missions aimed at detecting and characterizing Jupiter-and terrestrial-mass planets, it is critical that each target star be thoroughly vetted to determine whether it is a viable target given both the instrumental design and scientific goals of the program. With this in mind, we have conducted a high contrast imaging survey of mature AFGKM stars with the PALAO/PHARO instrument on the Palomar 200 inch telescope. The survey reached sensitivities sufficient to detect brown dwarf companions at separations of > 50 AU. The results of this survey will be utilized both by future direct imaging projects such as GPI, SPHERE and P1640 and indirect detection missions such as SIM Lite. Out of 84 targets, all but one have no close-in (0.45-1 ′′ ) companions and 64 (76%) have no stars at all within the 25 ′′ field-of-view. The sensitivity contrasts in the K s passband ranged from 4.5 to 10 for this set of observations. These stars were selected as the best nearby targets for habitable planet searches owing to their long-lived habitable zones (> 1 billion years). We report two stars, GJ 454 and GJ 1020, with previously unpublished proper motion companions. In both cases, the companions are stellar in nature and are most likely M dwarfs based on their absolute magnitudes and colors. Based on our mass sensitivities and level of completeness, we can place an upper limit of ∼17% on the presence of brown dwarf companions with masses >40 M J at separations of >1 arcsecond. We also discuss the importance of including statistics on those stars with no detected companions in their field of view for the sake of future companion searches and an overall understanding of the population of low-mass objects around nearby stars.

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Section: Data Reduction and Analysismentioning

confidence: 98%

Section: Data Reduction and Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A High-Contrast Imaging Survey ofSIM LitePlanet Search Targets

Tanner¹,

Gelino²,

Law³

2010

PUBL ASTRON SOC PAC

237

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“…There is also a more fundamental issue that must be considered: this survey is not the first to be sensitive to the presence of ULMCs, and a full treatment should consider all surveys that have properly reported null detections and detection limits (e.g. Sartoretti et al 1998;Massarotti et al 2005;Tanner et al 2007;Lafrenière et al 2008a;Metchev & Hillenbrand 2009;Chauvin et al 2010). Chauvin et al (2010) reported 1 detection (AB Pic) from 30-40 young solar-type targets surveyed (depending on the definitions of "young" and "solar-type").…”

Section: Companionsmentioning

confidence: 99%

Two Wide Planetary-Mass Companions to Solar-Type Stars in Upper Scorpius

Ireland

Kraus

Martinache

et al. 2010

ApJ

161

166

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At wide separations, planetary-mass and brown dwarf companions to solar type stars occupy a curious region of parameters space not obviously linked to binary star formation or solar-system scale planet formation. These companions provide insight into the extreme case of companion formation (either binary or planetary), and due to their relative ease of observation when compared to close companions, they offer a useful template for our expectations of more typical planets. We present the results from an adaptive optics imaging survey for wide (∼50-500 AU) companions to solar type stars in Upper Scorpius. We report one new discovery of a ∼14 M J companion around GSC 06214-00210, and confirm that the candidate planetary mass companion 1RXS J160929.1-210524 detected by Lafrenière et al. (2008b) is in fact co-moving with its primary star. In our survey, these two detections correspond to ∼4% of solar type stars having companions in the 6-20 M J mass and ∼200-500 AU separation range. This figure is higher than would be expected if brown dwarfs and planetary mass companions were drawn from an extrapolation of the binary mass function. Finally, we discuss implications for the formation of these objects. Subject headings: brown dwarfs, planetary systems, Infrared: planetary systems,

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“…Cc4 is listed in the Automated Plate Machine (APM) catalog, where its band r-band magnitudes are given as 21.13 mag and 19.15 mag, respectively. Tanner et al (2007) reported a visual companion of V 1171 Tau with a separation of 12. ′′ 7 and a position angle (PA) of 45.…”

Section: V1171 Taumentioning

confidence: 99%

Near-infrared imaging survey of faint companions around young dwarfs in the Pleiades cluster

Itoh

Oasa

Funayama

et al. 2011

Res. Astron. Astrophys.

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We conducted a near-infrared imaging survey of 11 young dwarfs in the Pleiades cluster using the Subaru Telescope and the near-infrared coronagraph imager. We found 10 faint point sources, with magnitudes as faint as 20 mag in the K-band, around 7 dwarfs. Comparison with Spitzer archive images revealed that a pair of the faint sources around V 1171 Tau are very red in the infrared wavelengths, indicative of very low-mass young stellar objects. However, the results of our follow-up proper motion measurements implied that the central star and the faint sources do not share common proper motions, suggesting that they are not physically associated.

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John S. Tanner Responds

Cited by 7 publications

References 0 publications

A High-Contrast Imaging Survey ofSIM LitePlanet Search Targets

A High-Contrast Imaging Survey ofSIM LitePlanet Search Targets

Two Wide Planetary-Mass Companions to Solar-Type Stars in Upper Scorpius

Near-infrared imaging survey of faint companions around young dwarfs in the Pleiades cluster

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