cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15156/bio/sh1284160.09fu
title: SH1284160.09FU

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-m0c5a5i
title: 16284

description: Recently a remarkable low surface brightness galaxy comma  NGC5846-UDG1 comma  was discovered in archival ground-based CFHT data. The galaxy has a low stellar mass (virgul10elev8 solar masses) comma  a large size (r_e=1.8 kpc) comma  and an unprecedented number of compact sources that resemble globular clusters. Keck spectroscopy confirms the association of the globular clusters and the diffuse lightdoublePoint they are at a common radial velocity of virgul2000 km-s comma  close to the group velocity of virgul1900 km-s. Based on the current ground-based imaging and spectroscopic data the galaxy might have up to 30% of its light in the form of globular clusters comma  significantly higher than any other galaxy known to date. Taking diffusion of low mass clusters into account comma  it is possible that the galaxy consisted solely of virgul100 globular clusters when it formed. Here we request 2 WFC3-UVIS orbits to study this extreme galaxy along with its unusual globular cluster system. With WFC3-UVIS we will measure the sizes comma  colors comma  ellipticities and luminosity function of the clusters. These properties will be compared to the globular cluster systems of other galaxies (and in particular other Ultra Diffuse Galaxies) comma  to determine whether NGC5846-UDG1.s globular clusters have similarities to those in other galaxies or represent something entirely new. We will also use the data to better determine the structure and morphology of this enigmatic galaxy in order to put further constraints on its dynamical state.
DOI: 10.15156/bio/sh1284161.09fu
title: SH1284161.09FU

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-m1jiaf2
title: 16935

description: Perform routine monitoring of NUV MAMA detector dark rate. The main purpose is  to look for evidence of a change in the dark rate comma  both to track on-orbit time  dependence and to check for a detector problem developing. Variations of count rates   as a function of orbital positions will be analyzed to study the effect of SAA.   Stacked images will help us study the spatial distribution of dark rates on the detector.
DOI: 10.57780/esa-m5kp88c
title: 16169

description: Life on Earth as we know it requires water and reliable access to phosphorus to drive basic biological processes. Studies of polluted white dwarf stars are able to detect both water and phosphorus in the accreted material from their extant planetary systems. In this proposal we seek to carefully examine the phosphorus content of a set of polluted white dwarf stars that are accreting the crust and mantle regions (the surface) of massive comma  differentiated rocky bodies. COS FUV spectroscopic observations of three white dwarf stars -- one water-rich and two relatively water-poor -- along with available data for another water-rich white dwarf will allow us to robustly assess their phosphorus content and compare the biological potential of very wet and more Earth-like worlds.
DOI: 10.15156/bio/sh1284162.09fu
title: SH1284162.09FU

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-m7vw8tv
title: 16563

description: The performance of MAMA microchannel plates can be monitored using a MAMA fold distribution procedure. The fold distribution provides a measurement of the distribution of charge cloud sizes incident upon the anode giving some measure of change in the pulse-height distribution of the MCP and comma  therefore comma  MCP gain. This proposal executes the same steps as the STIS MAMA Fold Distribution comma  Proposal 16356 comma  as Cycle 28.
DOI: 10.15156/bio/sh1284163.09fu
title: SH1284163.09FU

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-m95cr0l
title: 16552

description: Monitor wavelength calibration - dispersion solutions for STIS CCD modes. Internal wavecals will be obtained for representative wavelength settings with all 6 gratings (G230LB comma  G230MB comma  G430L comma  G430M comma  G750L comma  G750M) supported for use with the CCD.  All observations will be obtained with the HITM1 lamp comma  through the 52x0.1 aperture (which maps to 2 pixels at the CCD).
DOI: 10.57780/esa-ma0okv2
title: 17230

description: NUV imaging and spectroscopic acquisitions rely on the known separation between the astrophysical source and the calibration lamp as seen on the detector. That separation must be measured externally (on sky) and that has not been measured since SMOV. If that separation has changed and that change is not reflected in the flight software then NUV acquisitions would be off-center by the same amount. The principal effect of the unintended offset would be flux loss. Without the test we are hereby proposing we would not be able to distinguish this flux loss from other effects that factor into the Time Dependent Sensitivity (TDS) correction. After more than 12 years of lamp degradation it makes sense to check the separation. This one-time program tests that NUV acquisitions are still centered by comparing them to a lamp-independent flux-centered acquisition. The proposal description explains the observing design.  A more detailed descriptiondoublePoint This program compares the results of three different ways to do acquisitionsdoublePoint (1) ACQ-IMAGE comma  (2) NUV spectroscopic acq (ACQ-PEAKXD followed by ACQ-PEAKD) comma  and (3) manually computing the flux-weighted centroid after flux is vignetted by POSTARGs. After (1) and (2) we take verification spectra with the lamp on. These spectra can be used to measure the target-lamp separation. (3) is not really an acquisition but rather a simulation of an acquisition in the sense that we are collecting the data needed for flux centroiding comma  but the FSW will not actually compute the centroiding and move the telescope. I will compute the centroiding and compare it to where (1) and (2) placed the target. The reason for doing (3) is precisely because it does not use the lamp. Flux centroiding is a completely independent way of establishing where the center of the aperture is comma  and we can then compare it to (1) and (2) to see if the lamp-dependent methods are working. When the FSW executes a flux-centroided acquisition (NUV ACQ-SEARCH comma  NUV ACQ-PEAKD and all FUV acqs) the lamp is turned off. If the lamp were on its light would be a constant contribution to every dwell point comma  since the lamp does not get vignetted by POSTARG. That would just add floor counts which would then be subtracted by the centroiding algorithm comma  but the noise associated with it would remain.  For details on which FSW routines and parameters are involved see the ISR by Penton and Sahnow (2022 in prep.) and references therein.
DOI: 10.15156/bio/sh1284164.09fu
title: SH1284164.09FU

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-mbthv31
title: 17158

description: Faint dwarf galaxies are the observational bedrock of small-scale cosmology and galaxy formation. The faintest of these comma  the ultra-faint satellites of the Milky Way comma  are particularly informativedoublePoint as they have formed so few stars comma  they are very sensitive to the details of dark matter properties comma  feedback and reionization. While many models have been tuned to reproduce the Milky Way.s satellite population well comma  large variations between the luminosity functions of bright dwarfs in nearby groups coupled with theoretical expectations for variations in ultra-faint populations motivate searches for ultra-faint dwarfs in other groups.  Recent advances in wide-field deep multi-band imaging comma  star-galaxy separation and dwarf candidate search techniques place us in a position to explore this issue on a statistical footing. Sufficient data exists in five nearby galaxy groupsdoublePoint M31 comma  M81 comma  M64 comma  M83 and M94. We have identified 55 faint and ultra-faint satellite candidates using criteria designed to be as selective and restrictive as possible comma  while recovering artificial galaxies 3-10x deeper than current limits in these groups. We request 55 SNAPs with ACS and WFC3 in parallel (for local .background. estimation and legacy stellar halo science) to confirm a subset of this statistical sample. This program will confirm the faintest ever galaxy found outside the Milky Way comma  will allow measurement of their luminosities and sizes comma  will provide deep enough color-magnitude diagrams to constrain distance comma  metallicity and young stellar populations comma  and will propel robust Local Volume ultra-faint galaxy searches on an industrial scale with next-generation facilities like the Vera Rubin Observatory.
DOI: 10.15156/bio/sh1284165.09fu
title: SH1284165.09FU

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-mccsmp8
title: 16233

description: Planets form during the time comma  when the central star accretes material from the surrounding circumstellar disk and the final system architecture depends on the poorly known accretion and ejection history. Accretion tracers are particularly prominent in the UV so that the HST legacy program ULLYSES was conceived to obtain a UV atlas of accreting comma  young stars. In the UV comma  however comma  extinction is a severe issue and already moderate amounts of dust can completely extinguish any (accretion) signal. Accretion and extinction decline with age so that it is imperative to understand how well UV observations actually trace genuine accretion emission for higher absorption column densities or if rather other processes comma  namely jet emission or light scattered towards the observer by the upper disk layers comma  mimic accretion in spatially unresolved data such as the ULLYSES COS observations.  Our target comma  the classical T Tauri star AA Tau comma  currently experiences a long-lasting dimming event comma  presumably caused by inner disk dust comma  i.e. comma  the star is currently hidden behind a d_commanatural coronographd_comma and the direct emission is greatly reduced. Spatially unresolved HST COS data suggest that jet emission and scattering dominate the integrated FUV light during the dimming event. We propose to utilize this  situation to detect UV scattering for the first time and to measure the jet.s contribution to the FUV light through spatially resolving the emission with a series of STIS long-slit spectra. This experiment comma  right in time for ULLYSES comma  will uncover what fundamentally limits UV accretion studies comma  lack of signal due to absorption or d_commacontaminatingd_comma emission spoiling the interpretation of the signals.
DOI: 10.57780/esa-mhq94f3
title: 16587

description: Throughout the lifetime of WFC3 comma  a growing number of blobs (small comma  circular regions with slightly decreased sensitivity) have appeared in WFC3-IR images. Dark-Earth flats (observations of the dark side of the Earth) can be used to monitor the number and positions of blobs that appear in IR images due to dust on the channel select mechanism (CSM). These flats provide a high enough background level due to the dark-Earth airglow (virgul1000 DN - virgul3500 DN per pixel in each virgul25 second SPARS25 sample for F153M) which make the blobs easier to detect. By limiting the exposure time to 102.9 seconds comma  we avoid saturating the detector and yet will obtain several 25-sec samples to select from comma  in case some are contaminated by city lights. In addition to monitoring the number and positions of these blobs on the IR detector comma  this program will allow us to monitor the repeatability of WFC3.s channel select mechanism movements to ensure it does not exhibit anomalous behavior. More information can be found in WFC3 ISR 2018-06.
DOI: 10.15156/bio/sh1284166.09fu
title: SH1284166.09FU

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-mk5p5m7
title: 16893

description: The purpose of this program is to empirically determine the commanding overheads for WFC subarray modes comma  both unflashed and post-flashed. The commanding overheads are small periods of time comma  beyond the exposure time and any post-flash duration comma  over which dark current accrues. Though small comma  they impact dark correction and the pixel-based CTE model parameters.   Previous work on this topic used hot pixels in a small number of very short comma  unflashed subarray darks. The post-flashed subarray overheads were bootstrapped from full-frame overheads. Hot pixels are now known to fade with exposure time comma  and their dark rates are most uncertain-variable at short exposure times. We therefore wish to re-determine the empirical commanding overheads by obtaining 32 subarray dark frames with virgul340s darktime comma  half of which will be post-flashed to virgul55 e-. We will correct the hot pixels in these frames for their fading rates comma  using other data comma  to more accurately determine the commanding overheads.  We will take 16 subarray dark frames with 337s exposure time and no post-flash comma  using the WFC1B-1K. We will also take an identical set of subarray darks with 55e- post-flash.  All of the observations should be taken during the same anneal period and preferably within two days in order to avoid the appearance of many unstable hot pixels. The intent is for this CAL program to be scheduled nearly immediately (with the SMS currently being built) to help fill unused internal orbits during HST.s return to science with ACS.
DOI: 10.15156/bio/sh1284167.09fu
title: SH1284167.09FU

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-mkxxqy2
title: 16558

description: Monitor the wavelength calibration - dispersion solutions for representative wavelength settings of the STIS MAMA.  Internal wavecals will be obtained at primary and secondary central wavelengths for all the MAMA gratings -- chosen to cover both Cycle 29 usage and settings observed in previous monitoring programs (for long-term monitoring). Most of the settings in this program use the LINE lamp (for a total of approximately 1.5 hours)  two of the shortest wavelength settings use the somewhat brighter HITM2 lamp comma  however.  All but one setting will use a lamp current of 10 mA.
DOI: 10.57780/esa-mpbzd4b
title: 16336

description: This activity measures the baseline performance and commandability of the CCD subsystem. Only primary amplifier D is used. Bias and Flat Field exposures are taken in order to measure bias level comma  read noise comma  CTE comma  and gain. Numerous bias frames are taken to permit construction of d_commasuperbiasd_comma frames in which the effects of read noise have been rendered negligible. Full frame observations are made. Bias frames are taken in subarray readouts to check the bias level for ACQ and ACQ-PEAK observations.  All exposures are internals.