24 patients with malignant carcinoid tumours received octreotide and interferon alfa (IFN-alpha). All the patients initially received octreotide 50-100 micrograms, twice daily. When progressive ...symptoms or increasing biochemical markers were observed, the daily dose was raised to a median 300 micrograms. If the initial dose proved ineffective or if no improvement was seen after escalation, IFN-alpha was added (median 9 MU subcutaneously per week). After the addition of IFN-alpha, 17 of the 22 patients (77%) with elevated urinary 5-hydroxyindoleacetic acid showed a significant (> 50%) reduction. Only 1 patient progressed and 4 had continuously stable biochemical disease. No significant reduction in tumour size was noted; in 5 patients, the tumour continued to grow despite decreasing hormone levels. 18 patients had carcinoid syndrome when IFN-alpha was added in 10 (56%) symptoms ameliorated. Thus, the addition of IFN-alpha is beneficial for patients with malignant carcinoid tumours that progress and/or who do not respond to octreotide.
A computer-assisted morphometrical and microdensitometrical analysis has been performed on cardiovascular noradrenaline (NA), adrenaline (A) and neuropeptide (Y (NPY) neurons in adult and ...24-month-old male rats and on hypotensive (LL), normotensive (LN) and hypertensive (LH) male rats of the Lyon strain using the indirect immunoperoxidase procedures. It was found that in NPY/phenylethanolamine-N-methyltransferase (PNMT) costoring neurons of the CI area of the rostral medulla oblongata NPY-like immunoreactivity showed a more marked reduction than the PNMT immunoreactivity. Furthermore, within the parvocellular part of the paraventricular hypothalamic nucleus. NPY immunoreactive nerve terminal profiles were much more affected than the PNMT immunoreactive profiles during aging as revealed by a marked reduction in the number of profiles and by a marked reduction of absorbency values in the microdensitometrical analysis. Thus, in the NPY/PNMT costoring neurons of the A C1 group of the ventrolateral medulla projecting, for example, to the hypothalamus, the peptide transmission line may have a special vulnerability to the aging processes which may contribute to the development of hypertension in old people in view of a vasodepressor role of many central NPY/PNMT neurons. An extensive morphometrical and microdensitometrical analysis of the various catecholamine (CA) cell groups of the medulla oblongata of the LL, LN and LH rats of the Lyon strain was performed. In a comparison between LL and LH rats the A2 cell group of the LH strain showed a trend for an increase in the mean tyrosine hydroxylase (TH) immunoreactive cell body area and the C3 group showed a significant increase in the number of PNMT immunoreactive profiles.
High contrast imaging enables the determination of orbital parameters for substellar companions (planets, brown dwarfs) from the observed relative astrometry and the estimation of model and ...age-dependent masses from their observed magnitudes or spectra. Combining astrometric positions with radial velocity gives direct constraints on the orbit and on the dynamical masses of companions. A brown dwarf was discovered with the VLT/SPHERE instrument in 2017, which orbits at \(\sim\) 11 au around HD 206893. Its mass was estimated between 12 and 50 \(M_{Jup}\) from evolutionary models and its photometry. However, given the significant uncertainty on the age of the system and the peculiar spectrophotometric properties of the companion, this mass is not well constrained. We aim at constraining the orbit and dynamical mass of HD 206893 B. We combined radial velocity data obtained with HARPS spectra and astrometric data obtained with the high contrast imaging VLT/SPHERE and VLT/NaCo instruments, with a time baseline less than three years. We then combined those data with astrometry data obtained by Hipparcos and Gaia with a time baseline of 24 years. We used a MCMC approach to estimate the orbital parameters and dynamical mass of the brown dwarf from those data. We infer a period between 21 and 33{\deg} and an inclination in the range 20-41{\deg} from pole-on from HD 206893 B relative astrometry. The RV data show a significant RV drift over 1.6 yrs. We show that HD 206893 B cannot be the source of this observed RV drift as it would lead to a dynamical mass inconsistent with its photometry and spectra and with Hipparcos and Gaia data. An additional inner (semimajor axis in the range 1.4-2.6 au) and massive (\(\sim\) 15 \(M_{Jup}\)) companion is needed to explain the RV drift, which is compatible with the available astrometric data of the star, as well as with the VLT/SPHERE and VLT/NaCo nondetection.
Understanding the dominant brown dwarf and giant planet formation processes, and finding out whether these processes rely on completely different mechanisms or share common channels represents one of ...the major challenges of astronomy and remains the subject of heated debates. It is the aim of this review to summarize the latest developments in this field and to address the issue of origin by confronting different brown dwarf and giant planet formation scenarios to presently available observational constraints. As examined in the review, if objects are classified as "Brown Dwarfs" or "Giant Planets" on the basis of their formation mechanism, it has now become clear that their mass domains overlap and that there is no mass limit between these two distinct populations. Furthermore, while there is increasing observational evidence for the existence of non-deuterium burning brown dwarfs, some giant planets, characterized by a significantly metal enriched composition, might be massive enough to ignite deuterium burning in their core. Deuterium burning (or lack of) thus plays no role in either brown dwarf or giant planet formation. Consequently, we argue that the IAU definition to distinguish these two populations has no physical justification and brings scientific confusion. In contrast, brown dwarfs and giant planets might bear some imprints of their formation mechanism, notably in their mean density and in the physical properties of their atmosphere. Future direct imaging surveys will undoubtedly provide crucial information and perhaps provide some clear observational diagnostics to unambiguously distinguish these different astrophysical objects.
Aims. R Coronae Australis (R CrA) is the brightest star of the Coronet nebula of the Corona Australis (CrA) star forming region. It has very red colors, probably due to dust absorption and it is ...strongly variable. High contrast instruments allow for an unprecedented direct exploration of the immediate circumstellar environment of this star. Methods. We observed R CrA with the near-IR channels (IFS and IRDIS) of SPHERE at VLT. In this paper, we used four different epochs, three of them from open time observations while one is from the SPHERE guaranteed time. The data were reduced using the DRH pipeline and the SPHERE Data Center. On the reduced data we implemented custom IDL routines with the aim to subtract the speckle halo.We have also obtained pupil-tracking H-band (1.45-1.85 micron) observations with the VLT/SINFONI near-infrared medium-resolution (R~3000) spectrograph. Results. A companion was found at a separation of 0.156" from the star in the first epoch and increasing to 0.18400 in the final one. Furthermore, several extended structures were found around the star, the most noteworthy of which is a very bright jet-like structure North-East from the star. The astrometric measurements of the companion in the four epochs confirm that it is gravitationally bound to the star. The SPHERE photometry and the SINFONI spectrum, once corrected for extinction, point toward an early M spectral type object with a mass between 0.3 and 0.55 M?. The astrometric analyis provides constraints on the orbit paramenters: e~0.4, semi-major axis at 27-28 au, inclination of ~ 70{\deg} and a period larger than 30 years. We were also able to put constraints of few MJup on the mass of possible other companions down to separations of few tens of au.
Context. PDS 70 is a young (5.4 Myr), nearby (~113 pc) star hosting a known transition disk with a large gap. Recent observations with SPHERE and NACO in the near-infrared (NIR) allowed us to detect ...a planetary mass companion, PDS70b, within the disk cavity. Moreover, observations in H_alpha with MagAO and MUSE revealed emission associated to PDS70b and to another new companion candidate, PDS70c, at a larger separation from the star. Aims. Our aim is to confirm the discovery of the second planet PDS70c using SPHERE at VLT, to further characterize its physical properties, and search for additional point sources in this young planetary system. Methods. We re-analyzed archival SPHERE NIR observations and obtained new data in Y, J, H and K spectral bands for a total of four different epochs. The data were reduced using the data reduction and handling pipeline and the SPHERE data center. We then applied custom routines (e.g. ANDROMEDA and PACO) to subtract the starlight. Results. We re-detect both PDS 70 b and c and confirm that PDS70c is gravitationally bound to the star. We estimate this second planet to be less massive than 5 M Jup and with a T_eff around 900 K. Also, it has a low gravity with log g between 3.0 and 3.5 dex. In addition, a third object has been identified at short separation (~0.12") from the star and gravitationally bound to the star. Its spectrum is however very blue, so that we are probably seeing stellar light reflected by dust and our analysis seems to demonstrate that it is a feature of the inner disk. We, however, cannot completely exclude the possibility that it is a planetary mass object enshrouded by a dust envelope. In this latter case, its mass should be of the order of few tens of M_Earth. Moreover, we propose a possible structure for the planetary system based on our data that, however, cannot be stable on a long timescale.
The pre-main sequence star CHXR74 (M4.25) in ChaI was detected a few years ago to be a very low-mass spectroscopic binary. Determination of its mass would provide a valuable dynamical mass ...measurement at young ages in the poorly constrained mass regime of <0.3 Msun. We carried out follow-up radial velocity (RV) monitoring with UVES/VLT between 2008 and 2011 and high-resolution adaptive optic assisted imaging with NACO/VLT in 2008 with the aim to constrain the binary orbit. We present an orbital solution of the system based on the combined RV data set which spans more than 11 years of UVES monitoring for CHXR74. The best-fit Kepler model has an orbital period of 13.1 yrs, zero eccentricity, and a RV semi-amplitude of 2.2 km/s. A companion mass M2sini of 0.08 Msun is derived by using a model-dependent mass estimate for the primary of 0.24 Msun. The binary separation for i=90deg is 3.8 AU (23 mas). Complementary NACO images of CHXR74 were taken with the aim to directly resolve the binary. While there are marginal signs of an extended PSF, we have no convincing companion detected to CHXR74 in these images. From the non-detection of the companion together with a prediction of the binary separation at the time of the NACO observations, we derive an upper limit for the K-band brightness ratio of 0.5. This allows us to estimate an upper limit of the companion mass of 0.14 Msun by applying evolutionary models. Thus, we have confirmed that CHXR74 is a very low-mass spectroscopic binary and constrained the secondary mass to lie within the range of about 0.08 and 0.14 Msun. We predict an astrometric signal of the primary between 0.2 and 0.4 mas when taking into account the luminosity of the companion. The GAIA astrometric mission might well be able to solve the astrometric orbit of the primary and in combination with the presented RV data to determine an absolute companion mass.
Carcinoid tumours Tiensuu Janson, Eva M.; Oberg, Kjell E.
Baillière's clinical gastroenterology,
12/1996, Letnik:
10, Številka:
4
Journal Article
Carcinoid tumours offer a diagnostic and therapeutic challenge. Although new biochemical markers and improved methods for tumour detection, including PET and somatostatin receptor scintigraphy, have ...been developed during the last two decades many patients are still diagnosed at late stages of the disease. This is supported by the fact that the age of diagnosis is about the same today as it was 10 years ago. It is our opinion that plasma chromogranin A levels should be be determined in all patients which are investigated because of symptoms that might be connected to a neuroendocrine tumour. In cases with flushing or diarrhoea, U-5-HIAA should also be determined and these two tumour markers are enough to diagnose most patients with midgut carcinoid tumours. In patients with foregut or hindgut tumours other specific hormones should be included. For the localization procedure conventional radiological techniques including CT, MRI and ultrasound investigations should be supplemented with somatostatin receptor scintigraphy. Endoscopic ultrasound investigations might in the future be relevant for diagnosis of duodenal carcinoids, whereas gastric and rectal carcinoids are diagnosed by endoscopy. A combination of more aggressive surgery combined with medical treatment such as somatostatin analogues and α-interferon has significantly increased the survival rates in patients with classical midgut carcinoid tumours. Metastatic foregut and hindgut tumours are still a therapeutic challenge and it is important in the future to classify all carcinoid tumours based on specific tumour biology patterns. Such a tumour biology based treatment is a prerequisite for a more individually based therapy in the future.
