Jian Ge, Bo Zhao, Scott Powell, Ji Wang, Adam Fletcher, Liang Chang, John Groot, Xiaoke Wan, Hali Jakeman, Derek Myers, Elliot Grafer, Jian Liu, Frank Varosi, Sidney Schofield, Alexandria Moore, Maria-Ines van Olphen, Jordan Katz, Rory Barnes
This paper is to report the design and performance of a very high Doppler precision cross-dispersed
echelle spectrograph, EXtremely high Precision ExtrasolaR planet Tracker III (EXPERT-III), as part of a
global Exoplanet Tracker (ET) network. The ET network is designed to hunt low mass planets, especially
habitable rocky planets, around GKM dwarfs. It has an extremely high spectral resolution (EHR) mode of
R=110,000 and a high resolution (HR) mode of R=56,000 and can simultaneously cover 0.38-0.9 μm
with a 4kx4k back-illuminated Fairchild CCD detector with a single exposure. EXPERT-III is optimized
for high throughput by using two-prisms cross-disperser and a large core diameter fiber (2 arcsec on sky,
or 80 μm at f/4) to collect photons from the Kitt Peak National Observatory (KPNO) 2.1m telescope. The
average overall detection efficiency is ~6% from above the atmosphere to the detector for the EHR Mode
and about 11% for the HR mode. The extremely high spectral resolution in a compact design (the
spectrograph dimension, 1.34x0.8x0.48 m) is realized by coupling the single input 80 μm telescope fiber
into four 40 μm fibers and re-arranging the four small core diameter fibers into a linear fiber slit array (a
one-to-four fiber image slicer). EXPERT-III is operated in a vacuum chamber with temperature controlled
to ~2 milli-Kelvin rms for an extended period of time. The radial velocity (RV) drift is controlled to
within 10 meters/second (m/s) over a month. EXPERT-III can reach a photon noise limited RV
measurement precision of ~0.3 m/s for a V=8 mag GKM type dwarf with small rotation (vsini =2 km/s) in
a 15 min exposure. EXPERT-III’s RV measurement uncertainties for bright stars are primarily limited by
the Thorium-Argon (ThAr) calibration source (~0.5 m/s). EXPERT-III will serve as an excellent public
accessible high resolution optical spectroscope facility at the KPNO 2.1m telescope.
Silicon immersion gratings (SIGs) offer several advantages over the commercial echelle gratings for high
resolution infrared (IR) spectroscopy: 3.4 times the gain in dispersion or ~10 times the reduction in the
instrument volume, a multiplex gain for a large continuous wavelength coverage and low cost. We
present results from lab characterization of a large format SIG of astronomical observation quality. This
SIG, with a 54.74 degree blaze angle (R1.4), 16.1 l/mm groove density, and 50x86 mm2 grating area, was
developed for high resolution IR spectroscopy (R~70,000) in the near IR (1.1-2.5 μm). Its entrance
surface was coated with a single layer of silicon nitride antireflection (AR) coating and its grating surface
was coated with a thin layer of gold to increase its throughput at 1.1-2.5 m. The lab measurements have
shown that the SIG delivered a spectral resolution of R=114,000 at 1.55 m with a lab testing
spectrograph with a 20 mm diameter pupil. The measured peak grating efficiency is 72% at 1.55 m,
which is consistent with the measurements in the optical wavelengths from the grating surface at the air
side. This SIG is being implemented in a new generation cryogenic IR spectrograph, called the Florida IR
Silicon immersion grating spectrometer (FIRST), to offer broad-band high resolution IR spectroscopy
with R=72,000 at 1.4-1.8 um under a typical seeing condition in a single exposure with a 2kx2k H2RG IR
array at the robotically controlled Tennessee State University 2-meter Automatic Spectroscopic Telescope
(AST) at Fairborn Observatory in Arizona. FIRST is designed to provide high precision Doppler
measurements (~4 m/s) for the identification and characterization of extrasolar planets, especially rocky
planets in habitable zones, orbiting low mass M dwarf stars. It will also be used for other high resolution
IR spectroscopic observations of such as young stars, brown dwarfs, magnetic fields, star formation and
interstellar mediums. An optimally designed SIG of the similar size can be used in the Silicon Immersion
Grating Spectrometer (SIGS) to fill the need for high resolution spectroscopy at mid IR to far IR (~25-300 μm) for the NASA SOFIA airborne mission in the future.
We present a new concept for a Doppler imaging remote sensing instrument to track moving objects
within a wide field of view using a compact multi-object Dispersed Fixed-Delay Interferometer (DFDI).
The instrument is a combination of a Michelson type interferometer with a fixed optical delay and a
medium resolution spectrograph. This takes advantage of the strength of the DFDI approach over the
traditional cross-dispersed echelle spectrograph approach for high radial velocity (RV) precision
measurements: multi-object capability, high throughput and a compact design. The combination of a fiber
integral field unit (IFU) with a DFDI instrument allows simultaneous sampling of all of the objects within
the observing field of view (FOV) to provide differential RV measurements of moving objects over
background objects. Due to the three dimensional nature of the IFU spectroscopy the object location and
spectral features can be simultaneously acquired. With the addition of RV signals to the measurements,
this approach allows precise extraction of trajectories and spectral properties of moving objects (such as
space debris and near Earth Objects (NEOs)) through sequential monitoring of moving objects.
Measurement results from moving objects in a lab as well as moving cars in a field using this innovative
approach are reported.
Ultra-stable Monolithic Michelson interferometer can be an ideal reference for highprecision
applications such as RV measurement in planet searching and orbit study.
The advantages include wide wavelength range, simple sinusoidal spectral format,
and high optical efficiency. In this paper, we report that a monolithic Michelson
interferometers has been in-house developed with minimized thermal sensitivity with
compensation tuning. With a scanning white light interferometer, the thermal sensitivity is measured ~ 6x10-7/°C at 550 nm and it decreases to zero near 1000 nm.
We expect the wideband wavelength reference source to be stabilized better than 0.3 m/s for RV experiments
We present a fixed delay interferometer to be installed in IR-ET (Infra-Red Exoplanets Tracker). We introduce
the design, fabrication and testing processes. In particular, we present a new methodology of computing the
fundamental limit of radial velocity (RV) measurement given by photon noise for DFDI (Dispersed Fixed Delay
Interferometer) method as opposed to conventional echelle method. The new method is later used to determine
the optical path difference (OPD) of the IR-ET interferometer. In addition, we introduce a novel method
of monitoring the stability of the interferometer for IR-ET in broad-band using fourier-transform white-light
scanning interferometry technique. The new method can be potentially expanded and applied to thermo-optic
effect measurement if temperature control system is introduced into the experiment. The thermal response of
the optical system is 3500 m/s/°C. We find that the RV calibration precision of 'Bracketing' method is 1.74
m/s without temperature control.
Jian Ge, Bo Zhao, John Groot, Liang Chang, Frank Varosi, Xiaoke Wan, Scott Powell, Peng Jiang, Kevin Hanna, Ji Wang, Rohan Pais, Jian Liu, Liming Dou, Sidney Schofield, Shaun McDowell, Erin Costello, Adriana Delgado-Navarro, Scott Fleming, Brian Lee, Sandeep Bollampally, Troy Bosman, Hali Jakeman, Adam Fletcher, Gabriel Marquez
We report design, performance and early results from two of the Extremely High Precision Extrasolar
Planet Tracker Instruments (EXPERT) as part of a global network for hunting for low mass planets in the
next decade. EXPERT is a combination of a thermally compensated monolithic Michelson interferometer
and a cross-dispersed echelle spectrograph for extremely high precision Doppler measurements for nearby
bright stars (e.g., 1m/s for a V=8 solar type star in 15 min exposure). It has R=18,000 with a 72 micron
slit and a simultaneous coverage of 390-694 nm. The commissioning results show that the instrument has
already produced a Doppler precision of about 1 m/s for a solar type star with S/N~100 per pixel. The
instrument has reached ~4 mK (P-V) temperature stability, ~1 mpsi pressure stability over a week and a
total instrument throughput of ~30% at 550 nm from the fiber input to the detector. EXPERT also has a
direct cross-dispersed echelle spectroscopy mode fed with 50 micron fibers. It has spectral resolution of
R=27,000 and a simultaneous wavelength coverage of 390-1000 nm.
In high precision radial velocity (RV) measurements for extrasolar
planets searching and studies, a stable wide field Michelson
interferometer is very critical in Exoplanet Tracker (ET) instruments.
Adopting a new design, monolithic interferometers are homogenous and
continuous in thermal expansion, and field compensation and thermal
compensation are both satisfied. Interferometer design and fabrication are decrypted in details. In performance evaluations, field angle is typically 22° and thermal sensitivity is typically -1.7 x 10-6/°C, which corresponds to ~500 m/s /°C in RV scale. In interferometer stability monitoring using a wavelength stabilized laser source, phase shift data was continuously recorded for nearly seven days. Appling a frequent calibration every 30 minutes as in typical star observations, the interferometer instability contributes less than 1.4 m/s in RV error, in a conservative estimation.
We report performance of a new generation multi-object Doppler instrument for the on-going
Multi-object APO Radial-velocity Exoplanet Large-area Survey (MARVELS) of the Sloan
Digital Sky Survey III (SDSS-III) program. This instrument is based on dispersed fixed-delay
interferomtry design. It consists of a multi-object fiber-feed, a thermally compensated monolithic
fixed-delay interferometer, a high throughput spectrograph and a 4kx4k CCD camera. The
spectrograph resolving power is R=11,000 and the wavelength coverage is 500-570 nm. The
instrument is capable of measuring 60 stars in a single exposure for high to moderate precision
radial velocity (3-20 m/s) measurements depending on the star magnitudes (V=7.6-12). The
instrument was commissioned at the SDSS telescope in September 2008 and used to collect
science data starting in October 2008. Observations of reference stars show that the measured
photon noise limiting errors are consistent with the prediction for most of the measurements.
We report the design of a new generation multi-object high throughput Doppler instrument and
first light results at the Sloan Digital Sky Survey (SDSS) telescope. This instrument, capable of
simultaneously monitoring 60 stars for planet detection, is called the W.M. Keck Exoplanet
Tracker (or Keck ET) thanks to the generous gift from the W.M. Keck Foundation. It is designed
for a planet survey around hundreds of thousands of stars with V =8-13 for detecting tens of
thousands of planets in 2006-2020. The Doppler precision is between 3-25 m/s depending on the
star magnitude.
We also report a new planet detected with a prototype single object version ET instrument at the
KPNO Coude Feed/2.1 m telescopes. The extrasolar planet, ET-1 (HD 102195b), has a minimum
mass of 0.49 Jupiter masses and orbits a V = 8.1 G8V star with a 4.1 day period. The planet was
identified using the Coude Feed 0.9 meter telescope in spring 2005. This is the first time an
extrasolar planet around a star fainter than V=8 magnitude has been discovered with an under 1
meter size astronomical telescope and Doppler instrument. This planet discovery is possible due
to the extremely high throughput of the instrument, 49% measured from the fiber output end to
the detector.
A fiber feed system has been developed to allow a new generation multiple object Doppler instrument, called the WM Keck Exoplanet Tracker, simultaneously tracking 59 stars for high precision radial velocity measurements for planet detection, and switching among over 500 targets per night. The system includes 27 plug fiber bundles and 3 instrument fiber bundles, and each fiber bundle includes 22 fibers. Individual fibers of a plug fiber bundle are plugged to a plate to receive star lights, and then they are grouped together to form a compact 22-fiber connector. An instrument fiber bundle with a matching fiber bundle connector can connect and disconnect with the plug fiber bundle. The 45 m long instrument fiber bundles deliver the light from the telescope to an environment controlled instrument room in distance. We characterizes the light loses including the position and pointing error of plug connectors, the fiber end reflection, fiber misalignment at the mating connectors, focal ratio degradation and fiber absorption through the long fiber link. All fiber bundles are tested and average total throughput of 61% is achieved.
A new method for the monitoring of interferometer fiber optic sensors which utilizes a frequency-scanned fiber laser is investigated. The interrogation technique is based on the principle that if the laser frequency varies linearly with time, the optical signal reflected or transmitted is intensity-modulated at a frequency proportional to the optical path difference (OPD) in the interferometer. Fourier components in the detected optical output signal then correspond to the OPDs of any interferometers which have contributed to this modulation. The position of a peak in the power spectrum of this signal is proportional to the OPD of the interferometer responsible for that peak. Fine tuning of the OPD value is determined from the phase of the corresponding Fourier component. Experimentally, an Er:fiber laser scanned over a 46 nm range centered at 1545 nm was used to monitor intrinsic fiber Fabry-Perot interferometers (FFPIs). Variations in the laser scan rate were compensated using the optical signal modulated by a reference FFPI held at constant temperature. For three multiplexed sensors arranged in series, temperature was measured from 20°C to 610°C with a 0.02°C resolution.
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