Search

Erratum: Cepheid metallicity in the Leavitt law (C-metall) survey - I. HARPS-N@TNG spectroscopy of 47 classical Cepheids and 1 BL Her variables Keywords: errata; addenda; stars: abundances; stars: distances; stars: fundamental parameters; stars: variables: Cepheids; distance scale EN errata addenda stars: abundances stars: distances stars: fundamental parameters stars: variables: Cepheids distance scale 2887 2890 4 09/29/22 20221030 NES 221030 This is an erratum to the paper Cepheid metallicity in the Leavitt law (C-metall) survey - I. HARPS-N@TNG spectroscopy of 47 classical Cepheids and 1 BL Her variables, published in MNRAS, 2021, 508, 4047-4071. Errata, stars: abundances, stars: distances, stars: fundamental parameters, distance scale, addenda, stars: variables: Cepheids. [Extracted from the article]

Using Large Binocular Telescope deep imaging data from the Smallest Scale of Hierarchy Survey (SSH) and archival Hubble Space Telescope data, we reveal the presence of two elongated stellar features contiguous to a bar-like stellar structure in the inner regions of the dwarf irregular galaxy NGC 3741. These structures are dominated by stars younger than a few hundred Myr and collectively are about twice as extended as the old stellar component. These properties are very unusual for dwarf galaxies in the nearby Universe and difficult to explain by hydro-dynamical simulations. From the analysis of archival 21-cm observations, we find that the young stellar 'bar' coincides with an H  i high-density region proposed by previous studies to be a purely gaseous bar; we furthermore confirm radial motions of a few km s−1, compatible with an inflow/outflow, and derive a steeply rising rotation curve and high H  i surface density at the centre, indicating a very concentrated mass distribution. We propose that the peculiar properties of the stellar and gaseous components of NGC 3741 may be explained by a recent merger or ongoing gas accretion from the intergalactic medium, which caused gas inflows towards the galaxy centre and triggered star formation a few hundred Myr ago. This event may explain the young and extended stellar features, the bar-like structure, the very extended H  i disc and the central H  i spiral arms. The high central H  i density and the steeply rising rotation curve suggest that NGC 3741 may be the progenitor or the descendant of a starburst dwarf. [ABSTRACT FROM AUTHOR]

Classical Cepheids (DCEPs) are the most important primary indicators of the extragalactic distance scale. Establishing the dependence on metallicity of their period–luminosity and period–Wesenheit (PLZ / PWZ) relations has deep consequences on the calibration of secondary distance indicators that lead to the final estimate of the Hubble constant (H 0). We collected high-resolution spectroscopy for 47 DCEPs plus 1 BL Her variables with HARPS-N@TNG and derived accurate atmospheric parameters, radial velocities, and metal abundances. We measured spectral lines for 29 species and characterized their chemical abundances, finding very good agreement with previous results. We re-determined the ephemerides for the program stars and measured their intensity-averaged magnitudes in the V, I, J, H, K s bands. We complemented our sample with literature data and used the Gaia Early Data Release 3 (EDR3) to investigate the PLZ / PWZ relations for Galactic DCEPs in a variety of filter combinations. We find that the solution without any metallicity term is ruled out at more than the 5σ level. Our best estimate for the metallicity dependence of the intercept of the PLK s, PWJK s, PWVK s, and PWHVI relations with three parameters is −0.456 ± 0.099, −0.465 ± 0.071, −0.459 ± 0.107, and −0.366 ± 0.089 mag dex−1, respectively. These values are significantly larger than the recent literature. The present data are still inconclusive to establish whether or not also the slope of the relevant relationships depends on metallicity. Applying a correction to the standard zero-point offset of the Gaia parallaxes has the same effect of reducing by ∼22 per cent the size of the metallicity dependence on the intercept of the PLZ / PWZ relations. [ABSTRACT FROM AUTHOR]

We present results from an analysis of ∼29 000 RR Lyrae stars located in the Large Magellanic Cloud (LMC). For these objects, near-infrared time-series photometry from the VISTA survey of the Magellanic Clouds system (VMC) and optical data from the Optical Gravitational Lensing Experiment (OGLE) IV survey and the Gaia Data Release 2 catalogue of confirmed RR Lyrae stars were exploited. Using VMC and OGLE IV magnitudes we derived period–luminosity (PL), period–luminosity–metallicity (PLZ), period–Wesenheit (PW), and period–Wesenheit–metallicity (PWZ) relations in all available bands. More that  7000 RR Lyrae were discarded from the analysis because they appear to be overluminous with respect to the PL relations. The |$PL_{K_{\mathrm{s}}}$| relation was used to derive individual distance to |${\sim}22\, 000$| RR Lyrae stars, and study the three-dimensional structure of the LMC. The distribution of the LMC RR Lyrae stars is ellipsoidal with the three axis S 1 = 6.5 kpc, S 2 = 4.6 kpc, and S 3 = 3.7 kpc, inclination i  = 22 ± 4° relative to the plane of the sky and position angle of the line of nodes θ = 167 ± 7° (measured from north to east). The north-eastern part of the ellipsoid is closer to us and no particular associated substructures are detected and neither any metallicity gradient. [ABSTRACT FROM AUTHOR]

The Smallest Scale of Hierarchy (SSH) survey is an ongoing strategic large program at the Large Binocular Telescope, aimed at the detection of faint stellar streams and satellites around 45 late-type dwarf galaxies located in the Local Universe within ≃10 Mpc. SSH exploits the wide-field, deep photometry provided by the Large Binocular Cameras in the two wide filters g and r. This paper describes the survey, its goals, and the observational and data reduction strategies. We present preliminary scientific results for five representative cases (UGC 12613, NGC 2366, UGC 685, NGC 5477, and UGC 4426) covering the whole distance range spanned by the SSH targets. We reach a surface brightness (SB) limit as faint as μ(r) ∼ 31 mag arcsec−2 both for targets closer than 4–5 Mpc, which are resolved into individual stars, and for more distant targets through the diffuse light. Our analysis reveals the presence of extended low SB stellar envelopes around the dwarfs, reaching farther out than what traced by the integrated light, and as far out as, or even beyond, the observed H  i disc. Stellar streams, arcs, and peculiar features are detected in some cases, indicating possible perturbation, accretion, or merging events. We also report on the discovery of an extreme case of Ultra Diffuse Galaxy (μg(0) = 27.9 mag arcsec−2) in the background of one of our targets, to illustrate the power of the survey in revealing extremely low SB systems. [ABSTRACT FROM AUTHOR]

We present chemical abundances and radial velocities of six H  ii regions in the extremely metal-poor star-forming dwarf galaxy DDO 68. They are derived from deep spectra in the wavelength range 3500–10 000 Å, acquired with the Multi-Object Double Spectrograph at the Large Binocular Telescope (LBT). In the three regions where the [O  iii ] λ4363 Å line was detected, we inferred the abundance of He, N, O, Ne, Ar, and S through the 'direct' method. We also derived the oxygen abundances of all the six regions adopting indirect-method calibrations. We confirm that DDO 68 is an extremely metal-poor galaxy, and a strong outlier in the luminosity–metallicity relation defined by star-forming galaxies. With the direct method, we find indeed an oxygen abundance of 12+log(O/H) = 7.14 ± 0.07 in the northernmost region of the galaxy and, although with large uncertainties, an even lower 12 + log(O/H)  = 6.96 ± 0.09 in the 'tail'. This is, at face value, the most metal-poor direct abundance detection of any galaxy known. We derive a radial oxygen gradient of −0.06 ± 0.03 dex kpc−1 (or −0.30 dex |$R_{25}^{-1}$|⁠) with the direct method, and a steeper gradient of −0.12 ± 0.03 dex kpc−1 (or −0.59 dex |$R_{25}^{-1}$|⁠) from the indirect method. For the α-element to oxygen ratios, we obtain values in agreement with those found in other metal-poor star-forming dwarfs. For nitrogen, instead, we infer much higher values, leading to log(N/O)∼− 1.4, at variance with the suggested existence of a tight plateau at −1.6 in extremely metal-poor dwarfs. The derived helium mass fraction ranges from Y  = 0.240 ± 0.005 to Y  = 0.25 ± 0.02, compatible with standard big bang nucleosynthesis. Finally, we measured H  ii region radial velocities in the range 479−522  km  s−1 from the tail to the head of the 'comet', consistent with the rotation derived in the H  i. [ABSTRACT FROM AUTHOR]

We present intermediate-resolution (R ~ 1000) spectra in the ~3500-10 000 Å range of 14 globular clusters in the Magellanic irregular galaxy NGC 4449 acquired with the Multi- Object Double Spectrograph on the Large Binocular Telescope. We derived Lick indices in the optical and the Ca II triplet index in the near-infrared in order to infer the clusters' stellar population properties. The inferred cluster ages are typically older than ~9 Gyr, although ages are derived with large uncertainties. The clusters exhibit intermediate metallicities, in the range -1.2 ≲ [Fe/H] ≲ -0.7, and typically sub-solar [α/Fe] ratios, with a peak at ~-0.4. These properties suggest that (i) during the first few Gyr NGC 4449 formed stars slowly and inefficiently, with galactic winds having possibly contributed to the expulsion of the α-elements, and (ii) globular clusters in NGC 4449 formed relatively 'late', from a medium already enriched in the products of Type Ia supernovae. The majority of clusters appear also underabundant in CN compared to Milky Way halo globular clusters, perhaps because of the lack of a conspicuous N-enriched, second generation of stars like that observed in Galactic globular clusters. Using the cluster velocities, we infer the dynamical mass of NGC 4449 inside 2.88 kpc to be M(<2.88 kpc) = 3.15-0.75+3.16 x 109 M⊙. We also report the serendipitous discovery of a planetary nebula within one of the targeted clusters, a rather rare event. [ABSTRACT FROM AUTHOR]

We announce the discovery of K2-139 b (EPIC 218916923 b), a transiting warm-Jupiter (Teq = 547± 25 K) on a 29-d orbit around an active (logR ' HK =-4.46±0.06) K0V star in K2 Campaign 7.We derive the system's parameters by combining the K2 photometry with groundbased follow-up observations. With a mass of 0.387+0.083 -0.075 MJ and radius of 0.808+0.034 -0.033 RJ, K2-139 b is one of the transiting warm Jupiters with the lowest mass known to date. The planetary mean density of 0.91+0.24 -0.20 g cm-3can be explained with a core of ~50M⊗ . Given the brightness of the host star (V=11.653 mag), the relatively short transit duration (~5 h), and the expected amplitude of the Rossiter-McLaughlin effect (~25m s-1), K2-139 is an ideal target to measure the spin-orbit angle of a planetary system hosting a warm Jupiter. [ABSTRACT FROM AUTHOR]

We present the results of deep optical imaging of the radio/γ -ray pulsar PSR J2043+2740, obtained with the Large Binocular Telescope (LBT). With a characteristic age of 1.2Myr, PSR J2043+2740 is one of the oldest (non-recycled) pulsars detected in γ -rays, although with still a quite high rotational energy reservoir (Erot = 5.6 × 1034 erg s-1). The presumably close distance (a few hundred pc), suggested by the hydrogen column density (NH ≲ 3.6 × 1020 cm-2), would make it a viable target for deep optical observations, never attempted until now.We observed the pulsar with the Large Binocular Camera of the LBT. The only object (V = 25.44±0.05) detected within ∼3 arcsec from the pulsar radio coordinates is unrelated to it. PSR J2043+2740 is, thus, undetected down to V ∼26.6 (3σ), the deepest limit on its optical emission. We discuss the implications of this result on the pulsar emission properties. [ABSTRACT FROM AUTHOR]

In this paper we analyse the evolutionary status and properties of the old open cluster NGC 2355, located in the Galactic anticentre direction, as a part of the long-term programme Bologna Open Clusters Chemical Evolution. NGC 2355 was observed with the Large Binocular Camera at the Large Binocular Telescope using the Bessel B, V, and Ic filters. The cluster parameters have been obtained using the synthetic colour–magnitude diagram method, as done in other papers of this series. Additional spectroscopic observations with the Fibre-fed Echelle Spectrograph at the Nordic Optical Telescope of three giant stars were used to determine the chemical properties of the cluster. Our analysis shows that NGC 2355 has metallicity slightly less than solar, with [Fe/H]= −0.06 dex, age between 0.8 and 1 Gyr, reddening E(B − V) in the range 0.14–0.19 mag, and distance modulus (m − M)0 of about 11 mag. We also investigate the abundances of O, Na, Al, α, iron-peak, and neutron capture elements, showing that NGC 2355 falls within the abundance distribution of similar clusters (same age and metallicity). The Galactocentric distance of NGC 2355 places it at the border between two regimes of metallicity distribution; this makes it an important cluster for the study of the chemical properties and evolution of the disc. [ABSTRACT FROM AUTHOR]

STEP (the SMC in Time: Evolution of a Prototype interacting late-type dwarf galaxy) is a Guaranteed Time Observation survey being performed at the VST (the ESO VLT Survey Telescope). STEP will image an area of 74 deg2 covering the main body of the Small Magellanic Cloud (32 deg2), the Bridge that connects it to the Large Magellanic Cloud (30 deg2) and a small part of the Magellanic Stream (2 deg2). Our g, r, i, Hα photometry is able to resolve individual stars down to magnitudes well below the main-sequence turn-off of the oldest populations. In this first paper, we describe the observing strategy, the photometric techniques and the upcoming data products of the survey. We also present preliminary results for the first two fields for which data acquisition is completed, including some detailed analysis of the two stellar clusters IC 1624 and NGC 419. [ABSTRACT FROM AUTHOR]

Background Mycosis fungoides ( MF) is the most common type of cutaneous T-cell lymphoma; in its classical presentation it evolves slowly, but it can have an aggressive course in a subset of patients. Objectives To investigate the impact of epigenetic mechanisms on the progression of early stage MF. Methods We analysed DNA methylation at 12 different loci and long interspersed nucleotide elements-1 ( LINE-1), as a surrogate marker of global methylation, on tissue samples from 41 patients with stage I MF followed up for at least 12 years or until disease progression. The methylation profiles were also analysed in two T-cell lymphoma cell lines and correlated with gene expression. Results The selected loci were methylated in a tumour-specific manner; concomitant hypermethylation of at least four loci was more frequent in cases progressing within 1-3 and 3-6 years than in late-progressive or non-progressive cases. LINE-1 methylation was significantly lower in rapidly progressive MF at 3 years (61%, P < 0·001) than in those at 12 years (67%). PPARG, SOCS1 and NEUROG1 methylation showed remarkable differences among the prognostic groups, but only PPARG was a significant predictor of disease progression within 6 years, after adjustment for patients' age or gender. Strikingly, a methylation profile similar to progressive cases was found in highly proliferative Sézary-derived HUT78 cells but not in MF-derived HUT102 cells. Exposure to a DNA demethylating agent restored sensitivity to apoptosis and cell cycle arrest. Conclusions Epigenetic silencing of specific biomarkers can predict the risk of disease progression in early-stage MF, providing insights into its pathogenesis, prognosis and therapy. [ABSTRACT FROM AUTHOR]

ABSTRACT We present the analysis of the time series observations of CoRoT 102699796 obtained by the Convection, Rotation and planetary Transits ( CoRoT) satellite that show the presence of five independent oscillation frequencies in the range 3.6-5 c d−1. Using spectra acquired with FLAMES@VLT, we derive the following stellar parameters: spectral type F1V, Teff= 7000 ± 200 K, log ( g) = 3.8 ± 0.4, [M/H]=−1.1 ± 0.2, v sin i= 50 ± 5 km s−1, L/L⊙= 21+21− 11. Thus, for the first time we report the existence of a metal-poor, intermediate-mass pre-main-sequence (PMS) pulsating star. Ground-based and satellite data are used to derive the spectral energy distribution (SED) of CoRoT 102699796 extending from the optical to mid-infrared wavelengths. The SED shows a significant IR excess at wavelengths greater than ∼5 μm. We conclude that CoRoT 102699796 is a young Herbig Ae (F1Ve) star with a transitional disc likely associated with the H ii region [FT96]213.1-2.2. The pulsation frequencies have been interpreted in the light of the non-radial pulsation theory, using the losc code in conjunction with static and rotational evolutionary tracks. A minimization algorithm was used to find the best-fitting model with M= 1.84 M⊙, Teff= 6900 K which imply an isochronal age of t∼ 2.5 Myr. This result is based on the interpretation of the detected frequencies as g modes of low-moderate n-value. To our knowledge, this is the first time that such modes are identified in a intermediate-mass PMS pulsating star. Since CoRoT 102699796 lies in the region of the Hertzsprung-Russell (HR) diagram where the δ Sct and γ Dor instability strips intersect, we argue that the observed pulsation characteristics are intermediate between these classes of variables, i.e. CoRoT 102699796 is likely the first PMS hybrid γ Dor-δ Sct pulsator ever studied. [ABSTRACT FROM AUTHOR]

Located at the Galactic anticentre, Sh 2-284 is an H region that harbours several young open clusters. Dolidze 25, a rare metal-poor () young cluster, is one of these. Given its association with Sh 2-284, it is reasonable to assume a low metallicity for the whole H region. Sh 2-284 is expected to host a significant population of pre-main-sequence (PMS) stars of both low and intermediate mass (Herbig Ae stars). We aim to characterize these stars by means of a spectroscopic and photometric survey conducted with VIMOS@VLT and complemented with additional optical and infrared observations. In this survey we selected and characterized 23 PMS objects. We derived the effective temperature, the spectral energy distribution and luminosity of these objects, and, using theoretical PMS evolutionary tracks with the appropriate metallicity, we estimated the mass and the age of the studied objects. We also estimated a distance of 4 kpc for Sh 2-284, using the spectroscopic parallax of three OB stars. From the age determination we concluded that triggered star formation is occurring in this region. Our results show that a significant fraction of the young stellar objects (YSOs) may have preserved their disc/envelopes, in contrast with what is found in other recent studies of low-metallicity star-forming regions in the Galaxy. Finally, among the 23 bona fide PMS stars, we identified eight stars that are good candidates to be pulsators of the δ Scuti type. [ABSTRACT FROM AUTHOR]

Secukinumab shows high efficacy irrespective of HLA-Cw6 status in patients with moderate-to-severe plaque-type psoriasis: results from extension phase of the SUPREME study [8] Of these, 185 (42.6%) patients were I HLA-Cw6 i -positive (Cw6-POS), and 246 (56.7%) were I HLA-Cw6 i -negative (Cw6-NEG); Cw6 was not assessed for three patients. Cw6-NEG, HLA-Cw6 negative; Cw6-POS, HLA-Cw6 positive. gl. [Extracted from the article]