43 research outputs found
High-resolution broadband spectroscopy using externally dispersed interferometry at the Hale telescope: part 2, photon noise theory
High-resolution broadband spectroscopy at near-infrared (NIR) wavelengths (950 to 2450 nm) has been performed using externally dispersed interferometry (EDI) at the Hale telescope at Mt. Palomar, with the TEDI interferometer mounted within the central hole of the 200-in. primary mirror in series with the comounted TripleSpec NIR echelle spectrograph. These are the first multidelay EDI demonstrations on starlight. We demonstrated very high (10×) resolution boost and dramatic (20× or more) robustness to point spread function wavelength drifts in the native spectrograph. Data analysis, results, and instrument noise are described in a companion paper (part 1). This part 2 describes theoretical photon limited and readout noise limited behaviors, using simulated spectra and instrument model with noise added at the detector. We show that a single interferometer delay can be used to reduce the high frequency noise at the original resolution (1× boost case), and that except for delays much smaller than the native response peak half width, the fringing and nonfringing noises act uncorrelated and add in quadrature. This is due to the frequency shifting of the noise due to the heterodyning effect. We find a sum rule for the noise variance for multiple delays. The multiple delay EDI using a Gaussian distribution of exposure times has noise-to-signal ratio for photon-limited noise similar to a classical spectrograph with reduced slitwidth and reduced flux, proportional to the square root of resolution boost achieved, but without the focal spot limitation and pixel spacing Nyquist limitations. At low boost (∼1×) EDI has ∼1.4× smaller noise than conventional, and at >10× boost, EDI has ∼1.4× larger noise than conventional. Readout noise is minimized by the use of three or four steps instead of 10 of TEDI. Net noise grows as step phases change from symmetrical arrangement with wavenumber across the band. For three (or four) steps, we calculate a multiplicative bandwidth of 1.8:1 (2.3:1), sufficient to handle the visible band (400 to 700 nm, 1.8:1) and most of TripleSpec (2.6:1)
High-resolution broadband spectroscopy using externally dispersed interferometry at the Hale telescope: Part 1, data analysis and results
High-resolution broadband spectroscopy at near-infrared wavelengths (950 to 2450 nm) has been performed using externally dispersed interferometry (EDI) at the Hale telescope at Mt. Palomar. Observations of stars were performed with the “TEDI” interferometer mounted within the central hole of the 200-in. primary mirror in series with the comounted TripleSpec near-infrared echelle spectrograph. These are the first multidelay EDI demonstrations on starlight, as earlier measurements used a single delay or laboratory sources. We demonstrate very high (10×) resolution boost, from original 2700 to 27,000 with current set of delays (up to 3 cm), well beyond the classical limits enforced by the slit width and detector pixel Nyquist limit. Significantly, the EDI used with multiple delays rather than a single delay as used previously yields an order of magnitude or more improvement in the stability against native spectrograph point spread function (PSF) drifts along the dispersion direction. We observe a dramatic (20×) reduction in sensitivity to PSF shift using our standard processing. A recently realized method of further reducing the PSF shift sensitivity to zero is described theoretically and demonstrated in a simple simulation which produces a 350× times reduction. We demonstrate superb rejection of fixed pattern noise due to bad detector pixels—EDI only responds to changes in pixel intensity synchronous to applied dithering. This part 1 describes data analysis, results, and instrument noise. A section on theoretical photon limited sensitivity is in a companion paper, part 2
An EUV Study of the Intermediate Polar EX Hydrae
On 2000 May 5, we began a large multi-wavelength campaign to study the
intermediate polar, EX Hydrae. The simultaneous observations from six
satellites and four telescopes were centered around a one million second
observation with EUVE. Although EX Hydrae has been studied previously with
EUVE, our higher signal-to-noise observations present new results and challenge
the current IP models. Previously unseen dips in the light curve are
reminiscent of the stream dips seen in polar light curves. Also of interest is
the temporal extent of the bulge dip; approximately 0.5 in phase, implying that
the bulge extends over half of the accretion disk. We propose that the magnetic
field in EX Hydrae is strong enough (a few MG) to begin pulling material
directly from the outer edge of the disk, thereby forming a large accretion
curtain which would produce a very broad bulge dip. This would also result in
magnetically controlled accretion streams originating from the outer edge of
the disk. We also present a period analysis of the photometric data which shows
numerous beat frequencies with strong power and also intermittent and wandering
frequencies, an indication that physical conditions within EX Hya changed over
the course of the observation. Iron spectral line ratios give a temperature of
log T=6.5-6.9 K for all spin phases and a poorly constrained density of
n_e=10^10-10^11 cm^-3 for the emitting plasma. This paper is the first in a
series detailing our results from this multi-wavelength observational campaign.Comment: 27 pages, 7 figures, accepted for publication in Ap
Measuring the Boundary Layer and Inner Accretion Disk Temperatures for WX Ceti During Superoutburst
We obtained EUV photometry, optical spectroscopy, and multi-color optical
photometry for WX Cet during its 1998 November superoutburst. WX Cet is only
the second short-period, low mass transfer CV (TOAD) to ever be observed in the
EUV. Our determined superhump period is consistent with that found by Kato et
al. (0.059 d) and we confirm that superhumps are grey in the optical. The
optical spectra provide direct evidence that the line emission region is
optically thick and our multi-wavelength photometric measurements are used to
determine the inner accretion disk and boundary layer temperatures during
superoutburst. Using a determined distance to WX Cet of ~130 pc, we find
T= 21,000K and T_{BL}~72,500K. Both values are in good agreement with
that expected by models of the superoutburst continuum being produced by the
inner disk and boundary layer.Comment: Accepted in PASP - July 2002 issu
Implications of the SPEAR FUV Maps on Our Understanding of the ISM
The distribution of a low-density transition temperature (10^4.5 - 10^5.5 K)
gas in the interstellar medium conveys the character and evolution of diffuse
matter in the Galaxy. This difficult to observe component of the ISM emits
mainly in the far-ultraviolet (FUV) (912-1800 {\AA}) band. We describe spectral
maps of FUV emission lines from the highly ionized species CIV and OVI likely
to be the dominant cooling mechanisms of transition temperature gas in the ISM.
The maps were obtained using an orbital spectrometer, SPEAR, that was launched
in 2003 and has observed the FUV sky with a spectral resolution of \sim 550 and
an angular resolution of 10'. We compare distribution of flux in these maps
with three basic models of the distribution of transition temperature gas. We
find that the median distribution of CIV and OVI emission is consistent with
the spatial distribution and line ratios expected from a McKee-Ostriker (MO)
type model of evaporative interfaces. However, the intensities are a factor of
three higher than would be expected at the MO preferred parameters. Some high
intensity regions are clearly associated with supernova remnants and
superbubble structures. Others may indicate regions where gas is cooling
through the transition temperature.Comment: 6 pages, 2 figures, presented at "The Local Bubble and Beyond II,"
April 200
An optical fiber double scrambler and mechanical agitator system for the Keck planet finder spectrograph
We present the design and test results of a double-scrambler and fiber agitator system for the Keck Planet Finder (KPF) spectrograph. The mechanical agitator for modal noise suppression is constructed from two linear stages with the fibers mounted in a “W” curve. When driven back-and-forth at different rates, the stages change the position of the fiber curves, and hence vary the modes propagating through the fiber. Near-field temporal centroid shifts caused by modal-noise are reduced by a factor of 100 by the agitator, while mid-range spatial frequencies have reduced power by a factor of ∼300 in the near-field, and ∼1000 in the far-field. The scrambling system incorporates two octagonal fibers, and a scrambler consisting of two identical cemented lenses ∼20 cm apart, which exchanges the optical near- and far-fields of the fibers. The scrambler shows scrambling gains >16,000 in the near-field, and >40,000 in the far-field. The measured throughput efficiency of 99.3% of the expected maximum demonstrates that scrambler-induced focal ratio degradation (FRD) is minimal. The scrambler also serves as the feed-through into the vacuum chamber where the spectrograph is housed, thereby removing concerns about stressing the fibers, and introducing FRD, at this interface. Our illumination stabilization system, consisting of two octagonal fibers, a two lens scrambler, and a mechanical agitator, produces very homogeneous fiber output in both the near and far-fields. When coupled to the Keck Planet Finder spectrograph, this system provides illumination stability corresponding to a velocity of 0.30 m s^(−1)
The Three Dimensional Structure of EUV Accretion Regions in AM Herculis Stars: Modeling of EUV Photometric and Spectroscopic Observations
We have developed a model of the high-energy accretion region for magnetic
cataclysmic variables and applied it to {\it Extreme Ultraviolet Explorer}
observations of 10 AM Herculis type systems. The major features of the EUV
light curves are well described by the model. The light curves exhibit a large
variety of features such as eclipses of the accretion region by the secondary
star and the accretion stream, and dips caused by material very close to the
accretion region. While all the observed features of the light curves are
highly dependent on viewing geometry, none of the light curves are consistent
with a flat, circular accretion spot whose lightcurve would vary solely from
projection effects. The accretion region immediately above the WD surface is a
source of EUV radiation caused by either a vertical extent to the accretion
spot, or Compton scattering off electrons in the accretion column, or, very
likely, both. Our model yields spot sizes averaging 0.06 R, or the WD surface area, and average spot heights of 0.023
R. Spectra extracted during broad dip phases are softer than spectra
during the out-of-dip phases. This spectral ratio measurement leads to the
conclusion that Compton scattering, some absorption by a warm absorber,
geometric effects, an asymmetric temperature structure in the accretion region
and an asymmetric density structure of the accretion columnare all important
components needed to fully explain the data. Spectra extracted at phases where
the accretion spot is hidden behind the limb of the WD, but with the accretion
column immediately above the spot still visible, show no evidence of emission
features characteristic of a hot plasma.Comment: 30 Pages, 11 Figure
Comparison of Operative Mortality and Complications between Bronchoplastic Lobectomy and Pneumonectomy in Lung Cancer Patients
Bronchoplastic lobectomy is a lung-saving procedure indicated for central tumors, for which the alternative is pneumonectomy. We compared operative mortality and complications between bronchoplastic lobectomy and pneumonectomy in lung cancer patients. From March 1993 through December 2005, 1,461 patients were surgically resected for non-small cell lung cancer, including 73 who underwent bronchoplastic lobectomy and 258 who underwent pneumonectomy. Bronchoplastic lobectomy was performed on any lesion that could be completely resected by this technique, whereas pneumonectomy was only performed on lesions that could not be removed by bronchoplastic lobectomy. Operative deaths occurred in 1 of 73 (1.4%) bronchoplastic lobectomy and 26 of 258 (10.1%) pneumonectomy patients (p=0.014). Major complications occurred in 16 of 73 (21.9%) bronchoplastic lobectomy and 58 of 258 (22.5%) pneumonectomy patients (p=1.0). Bronchoplastic lobectomy has a lower risk of operative mortality than pneumonectomy. Although the complication rates were similar, bronchoplastic lobectomy was associated with improved postoperative cardiopulmonary status and a low prevalence of fatal complications after bronchial anastomosis. These findings indicate that bronchoplastic lobectomy is a valuable alternative to pneumonectomy for anatomically appropriate patients, regardless of underlying cardiopulmonary function
Spectro-interferometric observations of classical nova V458 Vul 2007
We used the Palomar Testbed Interferometer (PTI) to resolve 2.2 m
emission from the classical nova V458 Vul 2007 over the course of several days
following its discovery on 2007 August 8.54 UT. We also obtained K-band
photometric data and spectra of the nova during the early days of the outburst.
We also used photometric measurements from the AAVSO database. This is a unique
data set offering a 3-technique approach: high-resolution imaging, spectroscopy
and photometry. Our analysis shows that the nova ejecta can be modeled as an
inclined disk at low inclination i.e. low ellipticity which is consistent with
the nova being in the fireball phase at which the outflowing gas is optically
thick, confirmed by the presence of strong P-Cygni Balmer lines in the spectra.
The expansion velocity is 1700 , derived from the
H line. By combining the nova's angular expansion rate measured by PTI
with the expansion rate measured from spectroscopy, the inferred distance to
the nova is 9.9-11.4 kpc. We also used the K-band fluxes and the derived size
of the emission to estimate the total mass ejected from the nova . The quick transition of the nova from Fe II to He/N
class makes V458 Vul 2007 a hybrid nova.Comment: 31 pages, 7 figures, accepted for publication in Ap
An optical fiber double scrambler and mechanical agitator system for the Keck planet finder spectrograph
We present the design and test results of a double-scrambler and fiber agitator system for the Keck Planet Finder (KPF) spectrograph. The mechanical agitator for modal noise suppression is constructed from two linear stages with the fibers mounted in a “W” curve. When driven back-and-forth at different rates, the stages change the position of the fiber curves, and hence vary the modes propagating through the fiber. Near-field temporal centroid shifts caused by modal-noise are reduced by a factor of 100 by the agitator, while mid-range spatial frequencies have reduced power by a factor of ∼300 in the near-field, and ∼1000 in the far-field. The scrambling system incorporates two octagonal fibers, and a scrambler consisting of two identical cemented lenses ∼20 cm apart, which exchanges the optical near- and far-fields of the fibers. The scrambler shows scrambling gains >16,000 in the near-field, and >40,000 in the far-field. The measured throughput efficiency of 99.3% of the expected maximum demonstrates that scrambler-induced focal ratio degradation (FRD) is minimal. The scrambler also serves as the feed-through into the vacuum chamber where the spectrograph is housed, thereby removing concerns about stressing the fibers, and introducing FRD, at this interface. Our illumination stabilization system, consisting of two octagonal fibers, a two lens scrambler, and a mechanical agitator, produces very homogeneous fiber output in both the near and far-fields. When coupled to the Keck Planet Finder spectrograph, this system provides illumination stability corresponding to a velocity of 0.30 m s^(−1)