Byline: Kay Savage (1), Samuel Leung (2), S. Katrina Todd (1), Lindsay A. Brown (2), Robin L. Jones (3), David Robertson (1), Michelle James (1), Suzanne Parry (1), S. Maria Rodrigues Pinilla (4), ...David Huntsman (2), Jorge S. Reis-Filho (1) Keywords: Caveolin; Basal-like breast cancer; Prognosis; Western blot; Immunohistochemistry Background The aims of this study were to define the distribution of caveolin 2 (CAV2) in frozen and formalin fixed, paraffin embedded (FFPE) normal breast samples and the significance of CAV2 expression in breast cancer. Methods Caveolin 2 distribution in frozen and paraffin-embedded whole tissue sections of normal breast was evaluated using immunohistochemistry and immunofluorescence, in conjunction with antibodies to define luminal epithelial cells (oestrogen receptor and cytokeratin 8/18) and myoepithelial/ basal cells (cytokeratins 14 and 5/6, p63 and smooth muscle actin). CAV2 expression was also immunohistochemically analysed in two independent cohorts of invasive breast carcinomas (n = 245 and n = 418). Results In normal breast, CAV2 was expressed in myoepithelial cells, endothelial cells, fibroblasts and adipocytes. Luminal epithelial cells showed no or only negligible staining. CAV2 expression was observed in 9.6% of all breast cancers and was strongly correlated with high histological grade, lack of oestrogen receptor, progesterone receptor and cyclin D1 expression, and positivity for epidermal growth factor receptor, basal markers, p53 expression, and high proliferation index. Furthermore, CAV2 expression was significantly associated with basal-like immunophenotype and proved to be a prognostic factor for breast cancer-specific survival on univariate analysis. Conclusion Our results demonstrate that CAV2 is preferentially expressed in basal-like cancers and is associated with poor prognosis. Further in vitro studies are required to determine whether CAV2 has oncogenic properties or is only a surrogate marker of basal-like carcinomas. Author Affiliation: (1) The Breakthrough Breast Cancer Research Centre, Institute of Cancer Research, 237 Fulham Road, London, SW3 6JB, UK (2) Genetic Pathology Evaluation Centre, The Prostate Centre and Departments of Pathology of Vancouver Coastal Health Research Institute, British Columbia Cancer Agency, University of British Columbia, Vancouver, BC, Canada (3) Academic Biochemistry, The Royal Marsden Hospital Trust and Institute of Cancer Research, London, UK (4) Centro Nacional de Investigaciones Oncologicas, Madrid, Spain Article History: Registration Date: 28/07/2007 Received Date: 26/07/2007 Accepted Date: 27/07/2007 Online Date: 03/10/2007
AJ 167 243 (2024) We revisit the long-studied radial velocity (RV) target HD26965 using recent
observations from the NASA-NSF 'NEID' precision Doppler facility. Leveraging a
suite of classical ...activity indicators, combined with line-by-line RV analyses,
we demonstrate that the claimed 45-day signal previously identified as a planet
candidate is most likely an activity-induced signal. Correlating the bulk
(spectrally-averaged) RV with canonical line activity indicators confirms a
multi-day 'lag' between the observed activity indicator time series and the
measured RV. When accounting for this lag, we show that much of the observed RV
signal can be removed by a linear detrending of the data. Investigating
activity at the line-by-line level, we find a depth-dependent correlation
between individual line RVs and the bulk RVs, further indicative of periodic
suppression of convective blueshift causing the observed RV variability, rather
than an orbiting planet. We conclude that the combined evidence of the activity
correlations and depth dependence is consistent with a radial velocity
signature dominated by a rotationally-modulated activity signal at a period of
$\sim$42 days. We hypothesize that this activity signature is due to a
combination of spots and convective blueshift suppression. The tools applied in
our analysis are broadly applicable to other stars, and could help paint a more
comprehensive picture of the manifestations of stellar activity in future
Doppler RV surveys.
We present a dedicated transit and radial velocity survey of planets orbiting subgiant stars observed by the TESS Mission. Using $\sim$$16\( nights on Keck/HIRES, we confirm and characterize \)12\( ...new transiting planets -- \)\rm TOI-329\,b\(, \)\rm HD\,39688\,b\( (\)\rm TOI-480\(), \)\rm TOI-603\,b\(, \)\rm TOI-1199\,b\(, \)\rm TOI-1294\,b\(, \)\rm TOI-1439\,b\(, \)\rm TOI-1605\,b\(, \)\rm TOI-1828\,b\(, \)\rm HD\,148193\,b\( (\)\rm TOI-1836\(), \)\rm TOI-1885\,b\(, \)\rm HD\,83342\,b\( (\)\rm TOI-1898\(), \)\rm TOI-2019\,b\( -- and provide updated properties for 9 previously confirmed TESS subgiant systems (\)\rm TOI-197\(, \)\rm TOI-954\(, \)\rm TOI-1181\(, \)\rm TOI-1296\(, \)\rm TOI-1298\(, \)\rm TOI-1601\(, \)\rm TOI-1736\(, \)\rm TOI-1842\(, \)\rm TOI-2145\(). We also report the discovery of an outer, non-transiting planet, \)\rm TOI-1294\,c\( (\)P=160.1\pm2.5\( days, \)M_{\mathrm{p}}=148.3^{+18.2}_{-16.4} \,M_{\oplus}\(), and three additional stars with long-term RV trends. We find that at least \)19\pm8\%\( of subgiants in our sample of \)21\( stars have outer companions, comparable to main-sequence stars. We perform a homogeneous analysis of the stars and planets in the sample, with median uncertainties of \)3\%\(, \)8\%\( and \)15\%\( for planet radii, masses and ages, doubling the number of known planets orbiting subgiant stars with bulk densities measured to better than \)10\%$. We observe a dearth of giant planets around evolved stars with short orbital periods, consistent with tidal dissipation theories that predict the rapid inspiral of planets as their host stars leave the main sequence. We note the possible evidence for two distinct classes of hot Jupiter populations, indicating multiple formation channels to explain the observed distributions around evolved stars. Finally, continued RV monitoring of planets in this sample will provide a more comprehensive understanding of demographics for evolved planetary systems.
We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0 dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and ...confirmed with ground-based photometry (the Red Buttes Observatory 0.6m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet (\(\rho = 0.80^{+0.17}_{-0.15}\ \text{g cm}^{-3}\)) with a planetary radius of \(9.7 \pm \ 0.5 \ \text{R}_{\oplus}\) (\(0.87 \pm \ 0.04 \ \text{R}_{\text{Jup}}\)) and a planetary mass of \(135^{+17}_{-18} \text{M}_{\oplus}\) (\(0.42^{+0.05}_{-0.06} \ \text{M}_{\text{Jup}}\)). It has an orbital period of \(3.792622 \pm 0.000010\) days and an orbital eccentricity of \(0.06^{+0.07}_{-0.04}\). We measure a high metallicity for TOI-5344 of Fe/H = \(0.48 \pm 0.12\), where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of non-giants (\(\lesssim 8\ \text{R}_{\oplus}\)). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats.
The NEID spectrograph on the WIYN 3.5-m telescope at Kitt Peak has completed its first full year of science operations and is reliably delivering sub-m/s precision radial velocity measurements. The ...NEID instrument control system uses the TIMS package (Bender et al. 2016), which is a client-server software system built around the twisted python software stack. During science observations, interaction with the NEID spectrograph is handled through a pair of graphical user interfaces (GUIs), written in PyQT, which wrap the underlying instrument control software and provide straightforward and reliable access to the instrument. Here, we detail the design of these interfaces and present an overview of their use for NEID operations. Observers can use the NEID GUIs to set the exposure time, signal-to-noise ratio (SNR) threshold, and other relevant parameters for observations, configure the calibration bench and observing mode, track or edit observation metadata, and monitor the current state of the instrument. These GUIs facilitate automatic spectrograph configuration and target ingestion from the nightly observing queue, which improves operational efficiency and consistency across epochs. By interfacing with the NEID exposure meter, the GUIs also allow observers to monitor the progress of individual exposures and trigger the shutter on user-defined SNR thresholds. In addition, inset plots of the instantaneous and cumulative exposure meter counts as each observation progresses allow for rapid diagnosis of changing observing conditions as well as guiding failure and other emergent issues.
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