PHARO: A Near‐Infrared Camera for the Palomar Adaptive Optics System

By T. L. Hayward, B. Brandl, B. Pirger, C. Blacken, G. Gull, J. Schoenwald, J. Houck. 2001

181 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Aerospace Engineering

In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

Citations in the corpus

STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION (2015, methodology): “We obtained high resolution images of seven stars with the Palomar High Angular Resolution Observer (PHARO) infrared detector (Hayward et al. 2001) behind the PALM3000 adaptive optics system (Dekany et al. 2013) at the Palomar 5.1 m Hale telescope on the nights of 2015 February 3 and 4 UT. Sky…”
LOW FALSE POSITIVE RATE OF KEPLER CANDIDATES ESTIMATED FROM A COMBINATION OF SPITZER AND FOLLOW-UP OBSERVATIONS (2015, methodology): “These images were taken in the nearinfrared (J and K bands) with ARIES (McCarthy et al. 1998) on the MMT and PHARO (Hayward et al. 2001) on the Palomar Hale 200-inch.”
ALMOST ALL OF KEPLER'S MULTIPLE-PLANET CANDIDATES ARE PLANETS (2012, methodology): “…(KIC, Brown et al. 2011) with spectroscopic observations of the target and highresolution imaging, including Keck guider camera exposures and speckle imaging (Howell et al. 2011) and/or adaptive optics (Troy et al. 2000; Hayward et al. 2001), to search for other stars in the target aperture.”
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “To search for such a companion, we obtained direct imaging of HD126614A in J, H, and K-short (Ks) bands on the Hale 200” Telescope at Palomar Observatory on 13 April 2009 using the facility adaptive optics imager PHARO (Hayward et al. 2001).”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, methodology): “The Palomar campaign was conducted with the PALAO system (Troy et al. 2000) and the PHARO near-IR camera (Hayward et al. 2001) in its 25 mas pix−1 mode, providing a 25.6′′ × 25.6′′ FOV.”
THE KEPLER FOLLOW-UP OBSERVATION PROGRAM. I. A CATALOG OF COMPANIONS TO KEPLER STARS FROM HIGH-RESOLUTION IMAGING (2016, methodology): “The field of view of the ARIES instrument on the MMT was 20′′× 20′′, somewhat smaller than that of PHARO at Palomar, and the FWHM of the stellar images varied between about 0.1′′ and 0.6′′.”
Kepler-22b: A 2.4 EARTH-RADIUS PLANET IN THE HABITABLE ZONE OF A SUN-LIKE STAR (2011, methodology): “Near-infrared adaptive optics imaging of Kepler-22b was obtained on the night of 2010 July 3 UT with the Palomar Hale 5 m telescope and the Palomar High Angular Resolution Observer (PHARO) near-infrared camera (Hayward et al. 2001) behind the Palomar adaptive optics system (Troy et al. 2000).”
The Volume-limited A-Star (VAST) survey – I. Companions and the unexpected X-ray detection of B6–A7 stars (2011, methodology): “The data were acquired with several instruments listed in Table 3 – VisIm (Roberts & Neyman 2002) on AEOS, KIR (Doyon et al. 1998) on Canada–France–Hawaii Telescope (CFHT), NIRI (Hodapp et al. 2003) on Gemini-North and PHARO (Hayward et al. 2001) on Palomar.”
KEPLER-18b, c, AND d: A SYSTEM OF THREE PLANETS CONFIRMED BY TRANSIT TIMING VARIATIONS, LIGHT CURVE VALIDATION, WARM-SPITZER PHOTOMETRY, AND RADIAL VELOCITY MEASUREMENTS (2011, methodology): “Near-infrared adaptive optics imaging of K00137 was obtained on the night of 08 September 2009 UT with the Palomar Hale 5-m telescope and the PHARO nearinfrared camera (Hayward et al. 2001) behind the Palomar adaptive optics system (Troy et al. 2000).”
197 CANDIDATES AND 104 VALIDATED PLANETS IN K2's FIRST FIVE FIELDS (2016, result): “We also observed 33 stars with PHARO/PALM-3000 (Hayward et al. 2001; Dekany et al. 2013) at the 5 m Hale Telescope and 14 systems with LMIRCam at LBT (Leisenring et al. 2012), all at the K-band.”
MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS–AURIGA (2011, unknown): “All of our targets were observed with the facility AO imagers, Keck/NIRC2 (Matthews et al., in prep) and Palomar/PHARO (Hayward et al. 2001), which have aperture masks installed in cold filter wheels at or near the pupil stop.”
SN 2006gy: An Extremely Luminous Supernova in the Galaxy NGC 1260 (2006, methodology): “On UT 2006 Nov 1.3 we observed the event with the Adaptive Optics system (Troy et al. 2000) equipped with the Palomar High Angular Resolution Observer (Hayward et al. 2001) camera mounted on the Hale 5-m telescope.”
THE VECTOR VORTEX CORONAGRAPH: LABORATORY RESULTS AND FIRST LIGHT AT PALOMAR OBSERVATORY (2009, methodology): “We first conducted contrast measurements with PALAO and PHARO attached to the Cassegrain focus of the 5-m Hale telescope, and with PALAO locked on the internal white light source.”
KEPLER'S FIRST ROCKY PLANET: KEPLER-10b (2011, methodology): “Near-infrared adaptive optics imaging of KOI-72 was obtained on the night of 2009 September 8 UT with the Palomar Hale 200′′ telescope and the PHARO near-infrared camera (Hayward et al. 2001) behind the Palomar adaptive optics system (Troy et al. 2000).”
OBSERVATIONS OF HIERARCHICAL SOLAR-TYPE MULTIPLE STAR SYSTEMS (2015, methodology): “The PHARO camera uses a HgCdTe HAWAII detector for observations between 1 and 2.5 µm wavelength (Hayward et al. 2001).”