cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15156/bio/sh1284036.09fu
title: SH1284036.09FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.57780/esa-clbyurf
title: 16863

description: The standard CTE calibration observations involve imaging starfields to assess photometric and astrometric losses as a function of observation date comma  number of parallel transfers comma  background comma  star brightness comma  etc.  Like black holes comma  point sources d_commahave no haird_comma --- they have no distinguishing characteristics.  They can be characterized completely by the position and flux comma  and as such it is easy to come up with metrics for them and model how CTE impacts these metrics.  HST does indeed measure a lot of point sources comma  but it also measures a lot of resolved objectsdoublePoint  galaxies comma  nebulae comma  stars with disks comma  double stars comma  etc.  This 1-orbit program is an effort to examine the effect of CTE on resolved objects.    We will image a relatively dense galaxy field with WFC3-UVIS through the F606W filter.  This filter was chosen since we can get the best S-N in the quickest time.  We chose a galaxy field that was observed early in the lifetime of WFC3-UVIS comma  so that we can compare present-day comma  CTE-impacted observations against observations that should be largely free of CTE losses in order to investigate how much CTE affects resolved objects.  The end-product of this program will be an ISR that describes how CTE affects various galaxy d_commametricsd_comma.. FWHM.. integrated light. position.. etc.  We will also provide an image that shows an array of galaxy rasters and will indicate how imperfect CTE shuffles the pixel-to-pixel flux around.  This should help observers to better understand their data and proposers to better understand how best to plan their observations to ensure that what they want to measure can be measured.  This will also provide an interesting check on how well the pixel-based correction works on resolved objects comma  which should be easier to correct than stars comma  in that there is more self-shielding.
DOI: 10.15156/bio/sh1284037.09fu
title: SH1284037.09FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.57780/esa-cr8roaf
title: 16267

description: We request 18 orbits of HST time to observe the transit of HIP 41378 f comma  a Jovian planet (9.2 Earth radii) in a long-period orbit (542 days = 1.5 years) in a multi-planet system. The host star HIP 41378 is bright (Ks = 7.7 comma  V=8.9) comma  Sun-like (1.2 solar masses comma  1.3 solar radii) comma  and known to host at least five transiting planets. Two transits of HIP 41378 f were observed by the NASA K2 mission during non-consecutive three-month observing campaigns in 2015 and 2018 comma  restricting the set of possible periods to a set of harmonics with a maximum period of roughly 1000 days and a minimum period near 50 days. An intensive radial velocity campaign (464 observations spanning four years) has just ruled out the remaining possibilities comma  revealing that the HIP 41378 f has an orbital period of 542 days and an unexpectedly low mass of 12 Earth masses. HIP 41378 f is predicted to transit on 20 May 2021 and will not transit again until November 2022. We propose to observe the 2021 transit event with WFC3-G141 to accomplish three goalsdoublePoint (1) probe the atmospheric composition of a cool Jovian planet  (2) investigate the possible presence of rings  (3) place constraints on the presence of exomoons. HIP 41378 f occupies a poorly-probed region of parameter space and bridges the gap between the hotter planets previously studied via transmission spectroscopy and the cooler Jovian planets in our own solar system. HST transmission spectroscopy of HIP 41378 f would provide an opportunity to investigate the influence of stellar irradiation on giant planet atmospheres and inform efforts to detect Jupiter analogs with direct imaging surveys.
DOI: 10.57780/esa-czm648n
title: 16896

description: Ultra soft Narrow Line Seyfert  US-NLS are characterized by a large spectral variability comma  a very steep X-ray primary continuum  Gamma> 2.5 and a strong soft excess. This remarkable spectral shape questions the origin of their broad-band UV-X-ray continuum compared to standard Seyfert galaxies. We propose to perform a monitoring composed of 5x26 ks XMM observations totaldoublePoint 130ks comma  spaced by 2-3 days and coordinated with HST comma  to probe the FUV comma  of the US-NLS RX J1355.2+5612. The HST COS data are crucial to provide the best constraints on the accretion disc temperature which is expected to be quite hot in these objects. The proposed monitoring will then allow us to 1) disentangle the different spectral components present from the UV-FUV to X-ray energy range and 2) investigate the nature of the soft X-ray excess and discriminate between the theoretical models that have been heavily discussed in the past decade.
DOI: 10.15156/bio/sh1284038.09fu
title: SH1284038.09FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.57780/esa-d16zu2w
title: 16843

description: Using high-resolution observations from the Very Large Array comma  Reines et al. (2020) discovered a set of compact radio sources in nearby dwarf galaxies with luminosities indicative of accreting massive BHs. Moreover comma  many of these radio sources are not in the centers of the galaxies with offsets as large as virgul4.. (virgul2 kpc). We propose Chandra and HST observations of 8 dwarf galaxies hosting radio-selected massive BHs to 1) firmly establish the presence of massive BHs (some of which are 'wandering.) in these dwarf galaxies and characterize the compact X-ray emission from the BHs comma  2) place some constraints on the BH masses and Eddington ratios comma  and 3) search for stellar counterparts of the BHs and determine spatially-resolved star formation rates in the host galaxies.
DOI: 10.57780/esa-d1stndg
title: 16367

description: The Space Telescope Science Institute (STScI) Director has decided to devote up to 1000 orbits of Director.s Discretionary time in observing Cycles 27-29 to a new Hubble Ultraviolet Legacy program focused on star formation and associated stellar physics. This new program comma  ULLYSES (UV Legacy Library of Young Stars as Essential Standards) comma  will provide a UV spectroscopic reference sample of young (< 10 Myr) high- and low-mass stars. It will target over virgul150 OB stars in the Magellanic Clouds and lower metallicity galaxies in the Local Group comma  and virgul40 T Tauri stars and brown dwarfs in the Milky Way. In addition comma  ULLYSES will monitor 4 typical T Tauri stars over different rotational phases through at least three rotation periods comma  and over timescales of months to years. The resulting library will provide template spectra of massive stars at metallicities substantially below the well studied comma  while the low mass sample will cover a wide range of ages comma  accretion rates comma  and masses comma  including objects down to well below 0.5 M_sun. The legacy of this large UV dataset on the first 10 Myr of stellar evolution will be enhanced by complementary datasets obtained by the scientific community. In addition to the core goals of the program related to stellar astrophysics of low and high mass stars comma  this data will also enable exciting science in the fields of ISM comma  CGM comma  jets comma  and exoplanets. ULLYSES will be modeled after the Frontier Fields programdoublePoint all data obtained will be non-proprietary. The implementation team at STScI is developing high-level science data products and a sophisticated database and website for disseminating data from the ULLYSES program and ancillary datasets for the ULLYSES target sample from space and ground-based facilities.
DOI: 10.57780/esa-d371biv
title: 16289

description: Two broad scenarios have been suggested for the long-held problem of the formation of multiple populations (MPs) in Globular Clusters (GCs). According to the first option comma  GCs have experienced multiple star-formation episodes and provided a major contribution to the mass of the Galactic halo. As the alternative comma  there was a single star-formation episode comma  but a fraction of stars has successively accreted material processed and ejected by massive stars of the same generation. The mass functions (MFs) and the chemical composition of very-low mass M-dwarfs are the missing observational constraints to disentangle between the two scenarios. Historically comma  MPs in the GCs have been mostly investigated from UV and visual filters that are very sensitive to the bizarre chemical composition of the GC stars more massive than virgul0.6 solar masses. Due to the observational limits of the UV detectors comma  the faintest region of the color-magnitude diagram (CMD) is nearly unexplored. In the era of JWST comma  blind to the UV comma  the recent discovery comma  based on NIR HST photometry comma  of multiple sequences of very-low mass stars has provided a new window to study MPs. We propose to combine F110W and F160W photometry comma  which allows us to investigate the MPs phenomenon in the poorly-explored M-dwarf regime comma  with F275W comma  F336W comma  and F438W data comma  mandatory to explore the brightest region of the CMD. From the synergy of NIR comma  optical and UV photometry we will constrain the chemical composition of the MPs and derive for the first time their mass-functions in the interval between virgul0.1 and 0.8 solar masses. Our results will provide a major step forward to constrain the formation scenarios of MPs
DOI: 10.15156/bio/sh1284039.09fu
title: SH1284039.09FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.57780/esa-d3it41m
title: 16691

description: Supernovae and other stellar explosions (SNe) play key roles in galaxy formation and enrichment. Marking a stellar death comma  they are critical to understanding stellar evolution.  Cosmologists use SNe to measure the Universe.s expansion. Some SNe produce neutron stars and black holes. For these reasons and many others comma  including interesting physics of the explosions themselves comma  understanding the progenitors and explosions of all variety of SNe is of great importance to astrophysics.  Late-time (>200 days after explosion) HST observations of SNe measure the amount of radioactive material generated in the explosion and probe the circumstellar environments of the progenitor systems at radii inaccesible through other means. These same images can be used to examine the SN environment comma  and from nearby stars comma  we can constrain the progenitor star.s age. For all transients comma  these data reveal their late-time luminosity comma  constraining explosion physics and what powers them. These observations will also precisely determine the SN position comma  allowing future observations to search for companion stars. For SNe Iax comma  which are thought to not disrupt their white dwarf progenitor stars comma  we can detect the surviving star when leftover radioactive material forces it to the Eddington limit. Finally comma  late-time observations of TDEs can see the accretion disk hidden earlier.  We have assembled a sample of 75 recent comma  well-observed transients comma  that are sufficiently close that this science can be done with short HST exposures.  Combined with the statistical nature of these studies comma  this program is perfectly matched to snapshot observations.
DOI: 10.15156/bio/sh1284040.09fu
title: SH1284040.09FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.57780/esa-d4xbk97
title: 16765

description: We propose UV spectroscopy of the supermassive black hole binary (SBHB) candidate J095036+512838 (J0950) to test the alternative scenario that it harbors a perturbed accretion disk around a single black hole. By analogy to spectroscopic binary stars comma  this object was originally selected as a SBHB candidate by virtue of the virgul1300 km-s blueshift of its broad Balmer lines relative to the rest frame set by the narrow lines. According to new spectroscopic monitoring of the radial velocity curve comma  J0950 recently passed conjunction and is consistent with a SBHB with a period of order decades. This is an extremely strong indication of binary motion that no other candidate has shown before comma  making J095036 the strongest candidate of its class. The radial velocity curve also conclusively rules out the hypothesis that this is a recoiling black hole. We will observe the Ly-alpha and C IV broad lines to discriminate between the SBHB hypothesis and the single comma  perturbed accretion disk hypothesis. In the former scenario the UV lines are expected to be offset in velocity just as the optical Balmer lines while in the latter they are expected to be centered at the redshift of the narrow optical emission lines.
DOI: 10.57780/esa-dd7i2cg
title: 16436

description: The three nearly pure hydrogen WDs G191B2B comma  GD153 comma  and GD71 provide the basis of the HST flux calibrations for all the SIs. High fidelity models for each star are normalized with respect to the monochromatic flux of Vega at 5556A in order to establish standard candles in the sky. The flux of any star in the sky can be measured by the instrumental response relative to the ensemble response of these three fundamental standards.   Repeated observations of these 3 primaries can reveal any variability in one of the 3 primary WDs comma  as well as in our MAMA and CCD monitor standards comma  GRW+70 2824 and AGK+81 266. STIS should observe the primary WD triad with a cadence of every alternate year. Rather than putting .all our eggs in one basket. and depending only on single sensitivity monitoring stars comma  prudence suggest that return visits in low dispersion by STIS to the fundamental triad should be executed at something approaching the historic cadence. In addition to variability checks comma  each new observation adds to the statistical precision of the STIS flux calibration that is defined by these 3 stars. The brighter G191B2B requires only one orbit comma  because only the CCD can be used comma  while the fainter two standards require two orbits to obtain both MAMA and CCD spectra in low dispersion.  The standard data analysis produces Figures that illustrate the average change in response for the 5 STIS low dispersion modes in comparison to the triad of primary standards. The uncertainty in the STIS TDS correction is determined by the level of agreement between the triad of WDs and the respective monitoring standards.
DOI: 10.15156/bio/sh1284041.09fu
title: SH1284041.09FU

description: UNITE provides a unified way for delimiting, identifying, communicating, and working with DNA-based Species Hypotheses (SH). All fungal ITS sequences in the international nucleotide sequence databases are clustered to approximately the species level by applying a set of dynamic distance values (<0.5 - 3.0%). All species hypotheses are given a unique, stable name in the form of a DOI, and their taxonomic and ecological annotations are verified through distributed, web-based third-party annotation efforts. SHs are connected to a taxon name and its classification as far as possible (phylum, class, order, etc.) by taking into account identifications for all sequences in the SH. An automatically or manually designated sequence is chosen to represent each such SH. These sequences are released (https://unite.ut.ee/repository.php) for use by the scientific community in, for example, local sequence similarity searches and next-generation sequencing analysis pipelines. The system and the data are updated automatically as the number of public fungal ITS sequences grows.
DOI: 10.57780/esa-dfs2sg3
title: 16277

description: There are only two globular clusters where a modest investment of HST time can yield a high-precision measurement of trigonometric parallaxdoublePoint NGC6397 and M4. The parallax to NGC6397 has been measured successfully with HST to 2% uncertainty. An important HST legacy would be the completion of this pair comma  by measuring the M4 parallax while HST can still do so.  In the context of the Galaxy.s globular cluster system comma  these two clusters are complementary. NGC6397 is ancient (13 Gyr) and metal-poor (CORCHETE_OPENFe-HCORCHETE_CLOSE=-2.02) comma  while M4 is younger (11.5 Gyr) and of intermediate metallicity (CORCHETE_OPENFe-HCORCHETE_CLOSE=-1.15). NGC6397 is a frequent fiducial for stellar population models comma  while M4 hosts a rich set of RR Lyrae stars that can be used to better calibrate the period-luminosity relationship. The utility of each cluster as a population template and calibrator depends critically upon the distance uncertainties. The scarcity of population anchors in this regime is in contrast to the parameter space at younger ages (< 10 Gyr) and higher metallicities (CORCHETE_OPENFe-HCORCHETE_CLOSE > -1) comma  where many open clusters have high-precision parallaxes.  In a broader context comma  these two clusters represent an essential independent check on the parallaxes from the Gaia mission comma  which currently suffer from significant systematic errors on global comma  intermediate (20 degrees) comma  and small (1 degree) scales comma  hampering distances to the Galaxy.s globular clusters. If these errors are eventually resolved comma  HST parallaxes to globular clusters comma  independent of Gaia with distinct methodology comma  will provide an important validation. The observations we propose here will help anchor the distances to the entire globular cluster system of the Milky Way.
DOI: 10.6084/m9.figshare.22673488
title: Submarine channel stacking patterns controlled by the autogenic 3D kinematics of meander bends

description: S1: FLUMY model extended description, stacking pattern classification details, the methodology of channel point migration path measurements and centreline data
DOI: 10.6084/m9.figshare.22673488.v1
title: Submarine channel stacking patterns controlled by the autogenic 3D kinematics of meander bends

description: S1: FLUMY model extended description, stacking pattern classification details, the methodology of channel point migration path measurements and centreline data