432 research outputs found
Survival following surgical treatment for anorectal melanoma seems similar for local excision and extensive resection regardless of nodal involvement
Background: Anorectal melanoma is a rare malignancy with a dismal prognosis. The purpose of this study was to investigate whether the survival per stage is influenced by the surgical approaches (local excision or extensive resection), to assess prognostic factors of survival, and to answer the question whether the practiced surgical approaches changed over time. Methods: Dutch cancer registry organizations (IKNL and PALGA) were queried for all patients with a diagnosis of anorectal melanoma (1989-2019). Patients with disseminated disease at diagnosis were excluded. Survival outcomes were compared for the two surgical approaches stratified by stage (clinical node negative (cN0) and clinical node positive (cN+)) and date of diagnosis. Results: A total of 103 patients were included in this study. In both cN0 and cN+ patients the surgical strategy did not significantly influence survival (cN0: 21.7% 5-year survival, median 25 months for local excision versus 13.7% 5-year survival, median 17 months for extensive resection (p = 0.228), cN+: 11.1% 5-year survival for local excision, median 17 months versus 8.7% 5-year survival, median 14 months for extensive resection (p = 0.741)). Stage and date of diagnosis showed to be prognostic factors of survival. The ratio between the two surgical approaches was unchanged over three decades. Conclusions: Extensive resection does not seem to improve survival in both cN0 and cN+ anorectal melanoma patients compared to local excision. However in the past three decades no shift towards local excision has been found. cN+ stage and an older date of diagnosis are predictors for worse survival
Discovery of a high state AM CVn binary in the Galactic Bulge Survey
We report on the discovery of a hydrogen-deficient compact binary (CXOGBS
J175107.6-294037) belonging to the AM CVn class in the Galactic Bulge Survey.
Deep archival X-ray observations constrain the X-ray positional uncertainty of
the source to 0.57 arcsec, and allow us to uniquely identify the optical and UV
counterpart. Optical spectroscopic observations reveal the presence of broad,
shallow He i absorption lines while no sign of hydrogen is present, consistent
with a high state system. We present the optical lightcurve from Optical
Gravitational Lensing Experiment monitoring, spanning 15 years. It shows no
evidence for outbursts; variability is present at the 0.2 mag level on
timescales ranging from hours to weeks. A modulation on a timescale of years is
also observed. A Lomb-Scargle analysis of the optical lightcurves shows two
significant periodicities at 22.90 and 23.22 min. Although the physical
interpretation is uncertain, such timescales are in line with expectations for
the orbital and superhump periods. We estimate the distance to the source to be
between 0.5 - 1.1 kpc. Spectroscopic follow-up observations are required to
establish the orbital period, and to determine whether this source can serve as
a verification binary for the eLISA gravitational wave mission.Comment: Accepted for publication in MNRAS Letter
Open Questions in Classical Gravity
We discuss some outstanding open questions regarding the validity and
uniqueness of the standard second order Newton-Einstein classical gravitational
theory. On the observational side we discuss the degree to which the realm of
validity of Newton's Law of Gravity can actually be extended to distances much
larger than the solar system distance scales on which the law was originally
established. On the theoretical side we identify some commonly accepted but
actually still open to question assumptions which go into the formulating of
the standard second order Einstein theory in the first place. In particular, we
show that while the familiar second order Poisson gravitational equation (and
accordingly its second order covariant Einstein generalization) may be
sufficient to yield Newton's Law of Gravity they are not in fact necessary. The
standard theory thus still awaits the identification of some principle which
would then make it necessary too. We show that current observational
information does not exclusively mandate the standard theory, and that the
conformal invariant fourth order theory of gravity considered recently by
Mannheim and Kazanas is also able to meet the constraints of data, and in fact
to do so without the need for any so far unobserved non-luminous or dark
matter.Comment: UCONN-93-1, plain TeX format, 22 pages (plus 7 figures - send
requests to [email protected]). To appear in a special issue of
Foundations of Physics honoring Professor Fritz Rohrlich on the occasion of
his retirement, L. P. Horwitz and A. van der Merwe Editors, Plenum Publishing
Company, N.Y., Fall 199
The association between active tumor volume, total lesion glycolysis and levels of S-100B and LDH in stage IV melanoma patients
Introduction: The Standardized Uptake Value (SUV) in single lesions on F-18-FDG PET/CT scans and serum S-100B concentrations are inversely associated with disease-free survival in stage IV melanoma. The aim of this study was to assess the association between biomarkers (S-100B, LDH) and the PET-derived metrics SUVmean/max, metabolic active tumor volume (MATV), and total lesion glycolysis (TLG) in stage IV melanoma in order to understand what these biomarkers reflect and their possible utility for follow-up. Methods: In 52 stage IV patients the association between PET-derived metrics and the biomarkers S-100B and LDH was assessed and the impact on survival analyzed. Results: S-100B was elevated (>0.15 mu g/l) in 37 patients (71%), LDH in 11 (21%). There was a correlation between S-100B and LDH (R-2 = 0.19). S-100B was correlated to both MATV (R-2 = 0.375) and TLG (R-2 = 0.352), but LDH was not. Higher MATV and TLG levels were found in patients with elevated S-100B (p 250 U/l) (p <0.001). There was no association between the biomarkers and SUVmean/max. Survival analysis indicated that LDH was the only predictor of melanoma-specific survival. Conclusion: In newly diagnosed stage IV melanoma patients S-100B correlates with F-18-FDG PET/CT derived MATV and TLG in contrast to LDH, is more often elevated than LDH (71% vs. 21%) and seems to be a better predictor of disease load and disease progression. However, elevated LDH is the only predictor for survival. The biomarkers, S-100B and LDH appear to describe different aspects of the extent of metastatic disease and of tumornecrosis. (C) 2020 The Authors. Published by Elsevier Ltd
Author response to:Surgical treatment of anorectal melanoma: a systematic review and meta-analysis
A 180 Kpc Tidal Tail in the Luminous Infrared Merger Arp 299
We present VLA HI observations and UH88 deep optical B- and R-band
observations of the IR luminous merger Arp 299 (= NGC 3690 + IC 694). These
data reveal a gas-rich, optically faint tidal tail with a length of over 180
kpc. The size of this tidal feature necessitates an old interaction age for the
merger (~750 Myr since first periapse), which is currently experiencing a very
young star burst (~20 Myr). The observations reveal a most remarkable structure
within the tidal tail: it appears to be composed of two parallel filaments
separated by ~20 kpc. One of the filaments is gas rich with little if any
starlight, while the other is gas poor. We believe that this bifurcation
results from a warped disk in one of the progenitors. The quantities and
kinematics of the tidal HI suggest that Arp 299 results from the collision of a
retrograde Sab-Sb galaxy (IC 694) and a prograde Sbc-Sc galaxy (NGC 3690) that
occurred 750 Myr ago and which will merge into a single object in ~60 Myr. We
suggest that the present IR luminous phase in this system is due in part to the
retrograde spin of IC 694. Finally, we discuss the apparent lack of tidal dwarf
galaxies within the tail.Comment: LaTex, 14 pages, 11 figures, 4 tables, uses emulateapj.sty. Accepted
to AJ for July 1999. For version with full-resolution images see
http://www.cv.nrao.edu/~jhibbard/a299/HIpaper/a299HI.htm
The Molecule-Rich Tail of the Peculiar Galaxy NGC 2782 (Arp 215)
We present the first detection of a large quantity of molecular gas in the
extended tail of an interacting galaxy. Using the NRAO 12m telescope, we have
detected CO (1 - 0) at five locations in the eastern tail of the peculiar
starburst galaxy NGC 2782. The CO velocities and narrow (FWHM = 50 km/s) line
widths in these positions agree with those seen in HI, confirming that the
molecular gas is indeed associated with the tail rather than the main disk. As
noted previously, the gas in this tail has an apparent `counter-rotation'
compared to gas in the core of the galaxy, probably because the tails do not
lie in the same plane as the disk. Assuming the standard Galactic conversion
N(H2)/I(CO) factor, these observations indicate a total molecular gas mass of 6
X 10**8 M(sun) in this tail. This may be an underestimate of the total H2 mass
if the gas is metal-poor. This molecular gas mass, and the implied H2/HI mass
ratio of 0.6, are higher than that found in many dwarf irregular galaxies.
Comparison with an available H-alpha map of this galaxy, however, shows that
the rate of star formation in this feature is extremely low relative to the
available molecular gas, compared to L(H-alpha)/M(H2) values for both spiral
and irregular galaxies. Thus the timescale for depletion of the gas in this
feature is very long.Comment: 19 pages, 6 figures, Latex. To appear in the Astronomical Journa
The Hubble Space Telescope Key Project on the Extragalactic Distance Scale XXIV: The Calibration of Tully-Fisher Relations and the Value of the Hubble Constant
This paper presents the calibration of BVRIH$ Tully-Fisher relations based on
Cepheid distances to 21 galaxies within 25 Mpc, and 23 clusters within 10,000
km/s. These relations have been applied to several distant cluster surveys in
order to derive a value for the Hubble constant, H0, mainly concentrating on an
I-band all-sky survey by Giovanelli and collaborators which consisted of total
I magnitudes and 50% linewidth data for ~550 galaxies in 16 clusters. For
comparison, we also derive the values of H0 using surveys in B-band and V-band
by Bothun and collaborators, and in H-band by Aaronson and collaborators.
Careful comparisons with various other databases from literature suggest that
the H-band data, whose magnitudes are isophotal magnitudes extrapolated from
aperture magnitudes rather than total magnitudes, are subject to systematic
uncertainties. Taking a weighted average of the estimates of Hubble constants
from four surveys, we obtain H0 = 71 +- 4 (random) +- 7 (systematic) km/s/Mpc.
We have also investigated how various systematic uncertainties affect the value
of H0 such as the internal extinction correction method used, Tully-Fisher
slopes and shapes, a possible metallicity dependence of the Cepheid
period-luminosity relation and cluster population incompleteness bias.Comment: 34 pages, 13 figure
- …