cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.15156/bio/sh1283969.09fu
title: SH1283969.09FU

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-7s12jci
title: 16864

description: The IR grism flux monitor shows a sensitivity loss of 0.12+--0.01%-yr in G102 and 0.06+--0.01%-yr in G141. Observations of flux standards in the IR filters comma  however comma  show no evidence of any loss over time comma  but the repeatability is limited by systematic errors of +-- 1%. Scanned observations of M35 from 2015-2020 show marginal losses of 0.024+-- 0.008%-yr in F140W comma  but these data show a large scatter which may be related to detector preconditioning. Cluster observations allow for the measurement of many more stars comma  and photometry of the core Omega-Cen used for distortion monitoring suggests losses of 0.23 +-- 0.03%-yr in F160W comma  but crowding may play an effect on the results. Recent observations of a less dense stellar field in M4 in F110W suggest losses of 0.13 +-- 0.02%-yr  (first images only) and 0.20 +-- 0.03%-yr (all images) comma  but these consist of only 4 visits. We propose continued monitoring of M4 at a virgul6 month cadence. Two additional clusters are requesteddoublePoint the NGC104 field 6. from the core with F160W data from 2009-2013 and an Omega-Cen field 17. from the core with F110W  and  F160W images from 2016-2018 comma  both of which mimic the observation strategy from the respective preceeding epochs comma  to eliminate systematics from differing observing modes.
DOI: 10.57780/esa-7scqjx4
title: 16424

description: While AGN negative feedback on star formation has become a key ingredient on cosmic structure formation comma  the importance of AGN positive feedback comma  induced star formation from jet-cloud interaction comma  has also be realized. There are few direct examples of AGN positive feedback in the nearby universe. Recently comma  we have discovered potentially the closest example of AGN positive feedback in a nearby galaxy group where the radio jet of the central galaxy hits a spiral galaxy 154 kpc away in projection to trigger star formation at the side of interaction! As a rare and unique example important to study AGN positive feedback and SF conditions comma  we request a Chandra observation comma  along with joint time from VLA and HST comma  for the necessary multi-wavelength studies.
DOI: 10.15156/bio/sh1283970.09fu
title: SH1283970.09FU

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-7vtomr4
title: 16467

description: Knowledge of the COS Line Spread Function (LSF) is critical for users who wish to perform detailed line fitting studies as well as estimate signal-to-noise requirements. The exact shape of the LSF comma  and therefore the achievable overall spectral resolution comma  is a function of the overall optical path to a given lifetime position (LP). Here we determine the LSF and spectral resolution at LP5 for settings G130M-1291 and G130M-1327 comma  which encompass the range of cenwaves moving to LP5. We observe the SMC blue super giant AV 75 comma  whose spectra has both narrow interstellar absorption lines and complex broader convolved lines. We will test whether previous STIS E140M spectra of AV 75 convolved with model LP5 COS LSFs can reproduce the observed COS FUV spectra of numerous lines comma  thus validating the model spectra LSFs. We expect achieving a SN of about 60 for cenwave 1327 but possibly lower for 1291 comma  where the COS2025 policy prevents use of all four FP-POS comma  thus preventing mitigation of fixed pattern noise. We also take one exposure with cenwave G140L-800 at LP3 to 1) check the LP4 wavelength calibration accuracy at this mode and 2) use for a new derivation of the wavelength solution if needed. The 1291-FUVB data will also be used for the wavelength calibration derivation at LP5.
DOI: 10.57780/esa-7wo9jn9
title: 16161

description: Supernova shocks have been long-favored as sites for accelerating cosmic rays (CR). They have been studied extensively in multiple wavebands to look for signatures of accelerated particles in the strong amplified magnetic fields created at shock fronts. In this proposal comma  we present an optical-only study of CR acceleration comma  by examining a specific class of astrophysical shocks known as .Balmer shocks.. Our target is supernova remnant (SNR) 0519-69.0 in the Large Magellanic Cloud (LMC) that has strong Balmer emission. We propose a third ACS-WFC observation of this SNR comma  which will provide a virgul10 year baseline to measure the proper motion of the remnant. The well known distance to the LMC allows one to convert the proper motions to accurate shock velocities. The shock velocities comma  combined with ground-based spectroscopic measurements of the broad H alpha line-widths will be used to calculate the CR acceleration efficiency over a broad range of shock velocities using state-of-the-art models. We demonstrate the significant reduction in shock velocity uncertainties resulting from increasing the time baseline from the current 1 year to 10 years. We highlight the importance of matching the observational configuration to minimize systematic errors in the proper motion. With the new observation comma  we aim to reveal the dependence of CR acceleration efficiency on shock velocity.
DOI: 10.57780/esa-7xqv4up
title: 16978

description: Monitor the change in sensitivity over time with visits to the WD standard stars comma  GD71 comma  GD153 comma  G191B2B comma  and GRW+70 5824. Verify and refine the WFC photometric calibrations and repeatability measures. Single bright stars with photon statistical noise of virgul0.2% are a more precise and straightforward approach to measuring sensitivity changes than with the multitude of stars in 47 Tuc. This program has executed annually since Cycle 19.
DOI: 10.57780/esa-7z5dsn6
title: 16453

description: The local measurement of the Hubble constant comma  H0 comma  is now in tension with measurements from the distant universe by 4.4 sigma. The local H0 value is based on using Type Ia Supernovae (SNe Ia) as standard candles comma  calibrated from a small sample (<20) of nearby galaxies and limited by the (in)frequency of SN Ia events. One of the biggest improvements we can make in measuring H0 locally is to increase the number of calibrating systems.  A new SN Ia event has just occurred in the nearby galaxy NGC 4457 comma  estimated to be at virgul17 Mpc based on the light-curve. The host galaxy is close enough that a precision distance can be made using the tip of the red giant branch (TRGB) method. We propose ACS+WFC3 imaging of the resolved stars in the galaxy to precisely measure the distance and calibrate the SN Ia luminosity. A statistical sample of galaxies with SNe Ia and independent distance measurements is the ultimate goal for improving the local H0 measurement and such a sample is only built galaxy-by-galaxy when a nearby SN Ia occurs. In this context comma  NGC 4457 is a high priority target for a precision TRGB distance measurement.  In addition comma  the host-galaxy NGC 4457 is a more massive galaxy with little recent star formation. These properties are unique among SNe Ia calibrating systems but common in galaxies in the Hubble flow. SNe Ia in massive hosts standardize to a luminosity up to 10% brighter than those in lower mass hosts comma  a potential source of systematic uncertainty in the SN Ia distance scale. The new TRGB distance will provide an independent distance to a SN Ia in a galaxy with such properties and enable a comparison with SN Ia luminosity offsets estimated from galaxy redshifts.
DOI: 10.15156/bio/sh1283971.09fu
title: SH1283971.09FU

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-840hetw
title: 16416

description: This program acquires scanned observations for monitoring the relative changes in the WFC3-UVIS photometric throughput. The spectrophotometric white dwarf standard stars GD153 and GRW70 comma  and G-type star P330E comma  are scanned in a subset of filters periodically over the year. Historically comma  this program was intended as a monitor of the UV filters as they provide a means to detect contaminants on the instrument optics comma  with one or two visible-red filters serving as a control. Since then comma  additional filters in the visible and red have been added to the program to expand the monitor to longer wavelengths. The observing cadence is roughly once a month though some exceptions are required to accommodate visibilities.
DOI: 10.15156/bio/sh1283972.09fu
title: SH1283972.09FU

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-88wnuqu
title: 16834

description: (NotedoublePoint this is the HST part of a joint Chandra-HST projectdoublePoint the original Chandra proposal abstract follows.)  Chandra has been tracking coronal activity cycles of late-type stars via high-contrast soft X-rays comma  jointly with HST to capture UV tracers. Objective is to provide fundamental observational constraints for contemporary and future studies of the underlying magnetic Dynamo comma  whose inner workings remain elusive. The Sun.s high-energy modulations play an important d_commaSpace Weatherd_comma role in our heliosphere comma  as do stellar counterparts for their exoplanets. 3-year time-domain campaign (jointly with HST) is proposed for iconic Alpha Centauri comma  already followed by HRC-I since 2006. The Alpha Cen field also is rich in serendipitous sources comma  including flaring red dwarfs and several possibly cycling F-K stars.
DOI: 10.57780/esa-8e9g1s8
title: 16693

description: Radio-loud active galactic nuclei (RLAGN) are the most luminous radio sources in the Universe comma  and RLAGN at high-z are important for studying the formation of massive galaxies and supermassive black holes (SMBHs). The discovery of a radio galaxy at z=5.72 (TGSS J1530+1049) has pushed studies of RLAGN closer to the epoch of reionization (EoR). HST imaging of other high-z radio galaxies has shown that such systems are massive comma  with intense star-formation. They exhibit complex morphologies comma  large sizes and are frequently surrounded by overdensities of faint galaxies comma  indicative of a forming cluster environment. TGSS J1530+1049 at z=5.72 offers an opportunity to now investigate these phenomena at zvirgul6 comma  and we propose deep multi-band HST imaging with ACS and WFC3 to image the radio galaxy and its close companions comma  searching for overdensities on scales of 5 Mpc (co-moving) in its environment.  TGSS J1530+1049 is a JWST NIRCam GTO target and is the subject of an approved Cycle 1 NIRSpec-IFU program. It benefits from high-resolution VLBI radio imaging of its AGN jets and is an approved Chandra target. The combination of these proposed HST observations with JWST data will result in maps of the distribution of stellar mass and measurements of star-formation rate comma  dust comma  ionisation state and metallicity of the gas. Correlating the rest-UV morphology with AGN jets and constraining the evolutionary stage of the stellar populations are crucial to understand AGN feedback in massive galaxies near the EoR. Further comma  rest-frame UV HST imaging will allow the identification of any nearby companions through Lyman break selection comma  which will not be possible from the NIRCam data alone.
DOI: 10.57780/esa-8fpf9y3
title: 16848

description: HCG 40 comma  or Arp 321 comma  is a compact galaxy group with 5 cluster members. Member galaxies include an optical AGN and galaxies at a variety of star formation rates as measured in both UV and IR comma  though no Hubble data on these objects yet exists.  We propose to take broadband optical and H-alpha observations of HCG 40.
DOI: 10.15156/bio/sh1283973.09fu
title: SH1283973.09FU

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-8g3m0oz
title: 16213

description: The rest-UV emission line spectra of star-forming galaxies (SFGs) at z>6 serves as a primary tool to reveal the nature of ionizing sources that are responsible for the cosmic reionization. Low-metallicity star-forming dwarf galaxies at z<0.3 comma  show similar strong UV emission lines (eg  C IV comma  He II comma  O IIICORCHETE_CLOSE comma  and C IIICORCHETE_CLOSE) comma  and are being used to calibrate the UV diagnostics that can be applied to study galaxies in the reionization epoch. However comma  the high equivalent widths (EW > 20 Angstrom) seen for UV emission lines in z>6 galaxies comma  have not been observed in any of the local analogs. Such high EWs pose a challenge to the photoionization models comma  requiring the lowest metallicities comma  youngest stellar ages comma  and highest ionization parameters as model inputs to produce the required hard ionizing spectrum comma  and extreme emission lines. We propose to obtain HST COS (G140L) and STIS (G230L) spectra of a unique sample of 5 SFGs comma  recently identified as having extreme CORCHETE_OPENOIIICORCHETE_CLOSE-CORCHETE_OPENOIICORCHETE_CLOSE ratios (>22) with evidence for hard ionizing radiation from young comma  massive stars with ages < 3 Myrs. The photoionization models predict high nebular C IV and C IIICORCHETE_CLOSE EWs (> 15 Angstrom) comma  comparable to galaxies in the reionization epoch. Our goal is to (1) compare the fluxes and EWs of the UV emission lines to the model predictions and infer the ISM conditions comma  (2) calibrate the UV diagnostics that predict potential Lyman continuum escape comma  and (3) obtain constraints on the  ionizing sources (very massive stars comma  WR stars comma   or binaries) based on the hardness of the ionizing radiation. The results from our analysis of local analogs will offer crucial insights into the stellar populations and ISM conditions in extreme starbursts at high redshifts that are responsible for reionization.
DOI: 10.15156/bio/sh1283974.09fu
title: SH1283974.09FU

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-8j24vc8
title: 16461

description: Interest in low surface brightness galaxies (LSBGs) has experienced a renaissance in recent years. Intriguingly comma  a number of ultra diffuse galaxies comma  which are LSBGs with dwarf-like stellar masses spread over Milky Way-size areas comma  have been observed in the Coma cluster with extraordinarily large numbers (>40) of globular clusters (GCs). Since GC abundance correlates with galaxy dark matter halo mass for many galaxies comma  these LSBGs may have extremely high mass-to-light ratios. However comma  such GC-rich LSBGs have only been observed in high density comma  galaxy cluster environments. Can LSBGs in group environments have such extremely large GC systemsquestionMark We have just completed the first wide-field search for GC-rich LSBGs in Hyper Suprime-Cam data comma  with a focus on early-type comma  low-mass LSBGs. We request seven orbits of HST time to study the LSBGs with the largest GC-like point source excesses with imaging from the Advanced Camera for Surveys. With these data comma  we will be able to tightly constrain the GC abundances in our galaxies to determine whether they are truly the counterparts of the GC-rich LSBGs found in clusters. We will also constrain the GC luminosity functions of our LSBGs to compare to the most likely distances to our LSBGs. Finally comma  this HST data will provide verification of our ground-based GC search comma  which will provide invaluable insight for analyzing data from future telescopes like the Vera C. Rubin Observatory.
DOI: 10.57780/esa-8lp7yti
title: 16670

description: Truly massive galaxy clusters play a pivotal role for a wealth of extragalactic and cosmological research topics comma  and SNAPshot observations are ideally suited to identify the most promising targets for further comma  in-depth cluster studies. The power of this approach was demonstrated by ACS-WFC3 SNAPshots of X-ray selected MACS and eMACS clusters (at z>0.3 and z>0.5 comma  respectively) obtained in previous Cycles. Based on these data comma  the CLASH MCT comma  Hubble Frontier Fields comma  and RELICS legacy programs selected 60% of their targets from these surveys.   We propose to build upon the (e)MACS legacy SNAPshot programs by extending the surveyed redshift range to z=0.2 to create a volume-complete sample of highly X-ray luminous clusters at z=0.2-0.5. Our project will comma  for the first time comma  systematically explore the most massive clusters in the hugely promising z=0.2-0.3 range comma  which already gave us some of the most extreme clusters and cluster lenses known comma  e.g. comma  the Bullet Cluster comma  A1703 comma  RXJ1347-11 comma  and PLCK G171.9-40.7. By exploiting this barely tapped comma  rich resource comma   the proposed program will (a) identify yet more powerful gravitational telescopes for the next generation of in-depth studies of the distant Universe with HST and JWST comma  (b) provide tight constraints on the mass distribution within these extreme systems comma  (c) advance our understanding of the evolution and interactions of dark and luminous matter in cluster cores comma  and (d) unveil Balmer Break Galaxies at zvirgul2 and Lyman-break galaxies at z>6 as F814W dropouts.   Acknowledging broad community interest we waive our data rights for these observations.