233 research outputs found
Three photometric methods tested on ground-based data of Q 2237+0305
The Einstein Cross, Q~2237+0305, has been photometrically observed in four
bands on two successive nights at NOT (La Palma, Spain) in October 1995. Three
independent algorithms have been used to analyse the data: an automatic image
decomposition technique, a CLEAN algorithm and the new MCS deconvolution code.
The photometric and astrometric results obtained with the three methods are
presented. No photometric variations were found in the four quasar images.
Comparison of the photometry from the three techniques shows that both
systematic and random errors affect each method. When the seeing is worse than
1.0", the errors from the automatic image decomposition technique and the Clean
algorithm tend to be large (0.04-0.1 magnitudes) while the deconvolution code
still gives accurate results (1{sigma} error below 0.04) even for frames with
seeing as bad as 1.7". Reddening is observed in the quasar images and is found
to be compatible with either extinction from the lensing galaxy or colour
dependent microlensing. The photometric accuracy depends on the light
distribution used to model the lensing galaxy. In particular, using a numerical
galaxy model, as done with the MCS algorithm, makes the method less seeing
dependent. Another advantage of using a numerical model is that eventual
non-homogeneous structures in the galaxy can be modeled. Finally, we propose an
observational strategy for a future photometric monitoring of the Einstein
Cross.Comment: 9 pages, accepted for publication in A&
The Optical Gravitational Lensing Experiment. Monitoring of QSO 2237+0305
We present results from 2 years of monitoring of Huchra's lens (QSO
2237+0305) with the 1.3 m Warsaw telescope on Las Campanas, Chile. Photometry
in the V band was done using a newly developed method for image subtraction.
Reliable subtraction without Fourier division removes all complexities
associated with the presence of a bright lensing galaxy. With positions of
lensed images adopted from HST measurements it is relatively easy to fit the
variable part of the flux in this system, as opposed to modeling of the
underlying galaxy. For the first time we observed smooth light variation over a
period of a few months, which can be naturally attributed to microlensing. We
also describe automated software capable of real time analysis of the images of
QSO 2237+0305. It is expected that starting from the next observing season in
1999 an alert system will be implemented for high amplification events (HAE) in
this object. Time sampling and photometric accuracy achieved should be
sufficient for early detection of caustic crossings.Comment: 8 pages (including 4 figures and table), latex, emulateapj, submitted
to ApJ, revised version - minor change
An X-Ray Microlensing Test of AU-Scale Accretion Disk Structure in Q2237+0305
The innermost regions of quasars can be resolved by a gravitational-lens
{\lq}telescope{\rq} on scales down to a few AU. For the purpose, X-ray
observations are most preferable, because X-rays originating from the innermost
regions, can be selectively amplified by microlensing due to the so-called
`caustic crossing'. If detected, X-ray variations will constrain the size of
the X-ray emitting region down to a few AU. The maximum attainable resolution
depends mainly on the monitoring intervals of lens events, which should be much
shorter than the crossing time. On the basis of this idea, we performe
numerical simulations of microlensing of an optically-thick, standard-type disk
as well as an optically-thin, advection-dominated accretion flow (ADAF).
Calculated spectral variations and light curves show distinct behaviors,
depending on the photon energy. X-ray radiation which is produced in optically
thin region, exhibits intensity variation over a few tens of days. In contrast,
optical-UV fluxes, which are likely to come from optically thick region,
exhibit more gradual light changes, which is consistent with the microlensing
events so far observed in Q2237+0305.
Currently, Q2237+0305 is being monitored in the optical range at Apache Point
Observatory. Simultaneous multi-wavelength observations by X-ray sattelites
(e.g., ASCA, AXAF, XMM) as well as HST at the moment of a microlens event
enable us to reveal an AU scale structure of the central accretion disk around
black hole.Comment: 10 pages LaTeX, 3 figures, accepted to ApJ Letter. e-mail:
[email protected]
KIC7668647: a 14 day beaming sdB+WD binary with a pulsating subdwarf
The recently discovered subdwarf B (sdB) pulsator KIC7668647 is one of the 18
pulsating sdB stars detected in the Kepler field. It features a rich g-mode
frequency spectrum, with a few low-amplitude p-modes at short periods.
We use new ground-based low-resolution spectroscopy, and the near-continuous
2.88 year Kepler lightcurve, to reveal that KIC7668647 consists of a subdwarf B
star with an unseen white-dwarf companion with an orbital period of 14.2d. An
orbit with a radial-velocity amplitude of 39km/s is consistently determined
from the spectra, from the orbital Doppler beaming seen by Kepler at 163ppm,
and from measuring the orbital light-travel delay of 27 by timing of the many
pulsations seen in the Kepler lightcurve. The white dwarf has a minimum mass of
0.40 M_sun.
We use our high signal-to-noise average spectra to study the atmospheric
parameters of the sdB star, and find that nitrogen and iron have abundances
close to solar values, while helium, carbon, oxygen and silicon are
underabundant relative to the solar mixture.
We use the full Kepler Q06--Q17 lightcurve to extract 132 significant
pulsation frequencies. Period-spacing relations and multiplet splittings allow
us to identify the modal degree L for the majority of the modes. Using the
g-mode multiplet splittings we constrain the internal rotation period at the
base of the envelope to 46-48d as a first seismic result for this star. The few
p-mode splittings may point at a slightly longer rotation period further out in
the envelope of the star.
From mode-visibility considerations we derive that the inclination of the
rotation axis of the sdB in KIC7668647 must be around ~60 degrees.
Furthermore, we find strong evidence for a few multiplets indicative of
degree 3 <= L <= 8, which is another novelty in sdB-star observations made
possible by Kepler.Comment: arXiv admin note: text overlap with arXiv:1206.387
Kepler detection of a new extreme planetary system orbiting the subdwarf-B pulsator KIC10001893
KIC10001893 is one out of 19 subdwarf-B (sdB) pulsators observed by the
Kepler spacecraft in its primary mission. In addition to tens of pulsation
frequencies in the g-mode domain, its Fourier spectrum shows three weak peaks
at very low frequencies, which is too low to be explained in terms of g modes.
The most convincing explanation is that we are seeing the orbital modulation of
three Earth-size planets (or planetary remnants) in very tight orbits, which
are illuminated by the strong stellar radiation. The orbital periods are
P1=5.273, P2=7.807, and P3=19.48 hours, and the period ratios P2/P1=1.481 and
P3/P2=2.495 are very close to the 3:2 and 5:2 resonances, respectively. One of
the main pulsation modes of the star at 210.68 {\mu}Hz corresponds to the third
harmonic of the orbital frequency of the inner planet, suggesting that we see,
for the first time in an sdB star, g-mode pulsations tidally excited by a
planetary companion. The extreme planetary system that emerges from the Kepler
data is very similar to the recent discovery of two Earth-size planets orbiting
the sdB pulsator KIC05807616 (Charpinet et al. 2011a).Comment: 6 pages, 5 figures, accepted for publication in Astronomy and
Astrophysic
Three photometric methods tested on ground-based data of Q 2237+0305
The Einstein Cross, Q 2237+0305, has been photometrically observed in four bands on two successive nights at NOT (La Palma, Spain) in October 1995. Three independent algorithms have been used to analyse the data: an automatic image decomposition technique, a CLEAN algorithm and the new MCS deconvolution code. The photometric and astrometric results obtained with the three methods are presented. No photometric variations were found in the four quasar images. Comparison of the photometry from the three techniques shows that both systematic and random errors affect each method. When the seeing is worse than 1farcs0 , the errors from the automatic image decomposition technique and the Clean algorithm tend to be large (0.04-0.1 magnitudes) while the deconvolution code still gives accurate results (1sigma error below 0.04) even for frames with seeing as bad as 1farcs7 . Reddening is observed in the quasar images and is found to be compatible with either extinction from the lensing galaxy or colour dependent microlensing. The photometric accuracy depends on the light distribution used to model the lensing galaxy. In particular, using a numerical galaxy model, as done with the MCS algorithm, makes the method less seeing dependent. Another advantage of using a numerical model is that eventual non-homogeneous structures in the galaxy can be modeled. Finally, we propose an observational strategy for a future photometric monitoring of the Einstein Cross. Based on observations obtained at NOT, La Palma
Photometric Monitoring of the Gravitationally Lensed Ultraluminous BAL Quasar APM08279+5255
We report on one year of photometric monitoring of the ultraluminous BAL
quasar APM 08279+5255. The temporal sampling reveals that this gravitationally
lensed system has brightened by ~0.2 mag in 100 days. Two potential causes
present themselves; either the variability is intrinsic to the quasar, or it is
the result of microlensing by stars in a foreground system. The data is
consistent with both hypotheses and further monitoring is required before
either case can be conclusively confirmed. We demonstrate, however, that
gravitational microlensing can not play a dominant role in explaining the
phenomenal properties exhibited by APM 08279+5255. The identification of
intrinsic variability, coupled with the simple gravitational lensing
configuration, would suggest that APM 08279+5255 is a potential golden lens
from which the cosmological parameters can be derived and is worthy of a
monitoring program at high spatial resolution.Comment: 17 pages, with 2 figures. Accepted for publication in P.A.S.
Evidence for a source size of less than 2000 AU in Quasar 2237+0305
Recently, OGLE team have reported clear quasar microlensing signal in
Q2237+0305. We have analyzed the microlens event of ``image C'' by using their
finely and densely sampled lightcurves. From lightcurve fitting, we can
unambiguously set the source size of \lsim 0.98 Einstein Ring radius as a
conservative limit. This limit corresponds to , if we adopt
obtained by a recent statistical study of
mean mass of lens object. This gives a clear evidence for the existence of an
accretion disk in the central region of the quasar.Comment: 11 pages, including 1 table and 3 figures, accepted to ApJ
Spectroscopic Gravitational Lensing and Limits on the Dark Matter Substructure in Q2237+0305
Spatially resolved spectroscopic data from the CIRPASS integral field unit
(IFU) on Gemini are used to measure the gravitational lensing of the 4-image
quasar Q2237+0305 on different size scales. A method for measuring the
substructure present in the lens using observations at multiple wavelengths is
demonstrated to be very effective and independent of many of the degeneracies
inherent in previous methods. The magnification ratios of the QSO's narrow line
region (NLR) and broad line region (BLR) are measured and found to be disagree
with each other and with the published radio and mid-infrared magnification
ratios. The disagreement between the BLR ratios and the radio/mid-infrared
ratios is interpreted as microlensing by stars in the lens galaxy of the BLR
The disagreement between the radio/mid-infrared ratios and the NLR ratios is
interpreted as a signature of substructure on a larger scale, possibly the
missing small scale structure predicted by the standard cold dark matter (CDM)
model. Certain combinations of the radial profile and the substructure surface
densities are ruled out using extensive lensing simulations. A substructure
mass scale as large as 10^8 M is strongly disfavored while 10^4 M is too small
if the radio and mid-infrared emission regions have the expected sizes of ~10
pc. The standard elliptical isothermal lens mass profile is not compatible with
a substructure surface density of < 280 M/pc^2 at the 95% confidence level.
This is 4-7% of the galaxy's surface density (depending on which image position
is used to evaluate this). The required substructure surface density at the
required mass scale is high in comparison with the present expectations within
the CDM model.Comment: 29 pages, 16 figures, submitted to Ap
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