adsabs/AstroCLIMB huggingface dataset:
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces. Bottom row: the eccentricity distributions along the galacocentric distance r gal and metallicity distributions of HERSs. The positions of all NGC 3201/Arjuna stars are nearly identical in both phase and velocity space (see Figure 1), suggesting that they may originate from a GC. Another notable point is that I'itoi and Sequoia exhibit stable eccentricities around 0.7, with their r gal ranging from 6 to 15 kpc.
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in the V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces. Bottom row: the eccentricity distribution along the galacocentric distance r gal and metallicity distribution of Helmi streams. Most Helmi stream member stars show negative V  z  velocities, as well as metal-poor characteristics of MDF.
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in the V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces. Bottom row: the eccentricity distributions along the galacocentric distance r gal and metallicity distributions of the Low Energy Group. The Low Energy Group has very small median values for V  R , V  ϕ , V  x , and V  y , and they are −1.69 km s−1, 4.76 km s−1, −0.29 km s−1, and 1.47 km s−1 respectively. The MDF can be decomposed into three components, each with mean metallicity values [M/H] of approximately −1.29, −0.71, and −0.21 and corresponding weights of 19%, 61%, and 20%, respectively. The orange component with mean value −1.29 is in agreement with the distribution of the accreted region of the bulge in Horta’s work, related to Heracles (Horta et al. 2021).
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in the V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces. Bottom row: the eccentricity distributions along the galactocentric distance r gal, the metallicity distributions of the hot thick disk, and the Toomre diagram. The hot thick disk is situated at the ends of the banana-shaped arc in the the V  X −V  y  plane. The close attachment to the curve where ∣V−V LSR∣ = 210 km s−1 is also visible in the bottom right panel.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The comparison of cluster candidates found in this study and confirmed in the X-ray observation. The overdensity significance represents the number of standard deviations by which the density field deviates from its mean. Upper panel: the clusters that we identify have significant overdensities by definition, while X-ray groups are more likely to be less dense and comprise a small number of member galaxies. Lower panel: the matched clusters show a statistical correlation (Pearson correlation coefficient = 0.55) between the total stellar mass of member galaxies and halo mass estimated from X-ray detected groups. The best-fit linear regression between the two masses among cluster candidates is displayed as a black dashed line.
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in the V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces. Bottom row: the eccentricity distributions along the galacocentric distance r gal and metallicity distributions of PG1 and PG2. PG1 exhibits disklike orbital properties, yet it features higher eccentricities, predominantly ranging from 0.4 to 0.6, along with a wide metallicity distribution. PG2 demonstrates Aleph-like kinematics and presents a natural transition within the eccentricity-r gal space, suggesting that it may represent the high eccentricity and inner portion of the Aleph structure.
Paper: Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Authors: Haoyang Liu, Cuihua Du, Dashuang Ye, Jian Zhang, Mingji Deng
Figure caption: Top row: the velocity distributions in the V  R −V  ϕ , V  R −V  x , and V  x −V  y  spaces. Most Thamnos members have slight ∣V  ϕ ∣ and have both positive and negative V  z . Bottom row: the eccentricity is ranging broadly from ∼0.35 to ∼0.85, with a visible metal-poor characteristic shown in MDF (the MDF of NGC 5139 is also shown for comparison).
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The distribution of quiescent galaxy fraction and redshift in the mass-limited sample. The error bars represent the 68% confidence interval obtained from 1000 iterations of determining the membership by adding the error to the redshift center of the cluster. The errors follow a normal distribution N(0, σ(1 + z)), where σ(1 + z) corresponds to the photometric redshift uncertainty at a given redshift. For comparison, the quiescent galaxy fraction from the field is overlaid with a dashed line.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: Photometric redshift uncertainty (NMAD, σ Δz/1+z ) as a function of photometric redshift (red line). The uncertainty is calculated by comparing photometric redshift derived from LePHARE with the publicly available spectroscopic redshift catalog (S. J. Lilly et al. 2007). The background 2D histogram shows the population of galaxies within the photometric redshift and uncertainty bins.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: Mass complete limit as a function of photometric redshift. The blue solid line represents the mass complete limit of all types of galaxies while the red solid line is for quiescent galaxies only. The blue and red dashed lines indicate the mass completeness limits for all types and quiescent galaxies at = 1.4. We used galaxies exceeding the stellar mass limit as indicated by the blue dashed line. The background 2D histogram stands for the number of galaxies in a given redshift and stellar mass bin.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The median QF (upper panel) and median sSFR (lower panel) in each stellar mass bin of member galaxies. The member galaxies in clusters with FoF fractions larger than the median at a given redshift bin (open red star) are more actively forming stars than those in clusters with lower FoF fractions (open blue triangle). The filled green cross represents the case of field galaxies that are residing in the area with density ≤2σ for reference. The observational data from other literature (A. Muzzin et al. 2012; L. Lin et al. 2014) are overplotted in gray points. Here, we only compare the face values of the sSFR and the QF to see if their general trends with regard to stellar masses are consistent. Note that the criteria of quiescent/star-forming galaxies, environment (field, group, and cluster), and initial mass function (IMF) models are different between studies.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: Examples of overdense areas showing how the FoF fraction is defined. Each panel displays overdensities (red region) connected to host cluster candidates (filled black square) in increasing order of QF (left to right). The FoF fraction is defined as the ratio of the red area to the whole area (gray+red+pink areas). Unconnected overdensities within a 2 Mpc linking length are depicted in the pink region.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The anticorrelation between the QF and FoF fraction in 4 redshift bins. The Pearson correlation coefficient and its associated p-value are denoted as ρ and p  h , respectively, where the subscript h signifies fixed halo masses. The halo mass is represented as a color of marker. The star-shaped markers correspond to the clusters that have been detected in the X-ray group catalog (G. Gozaliasl et al. 2019) while those in square shape are candidates found based on photometric redshifts in this study.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The median QF of host galaxy clusters (pink circle), galaxies in infalling groups (filled blue square), infalling galaxies (filled orange triangle), and total infallers (galaxies + groups, filled green cross) at a given snapshot (redshift). The member galaxy ratio, represented as blue (groups) and orange (galaxies) shades, shows the number of infalling galaxies/groups divided by the number of cluster members before the accretion of the galaxies/groups.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The x-axis denotes the 2D projected cylindrical FoF fraction in the light-cone mock catalog (A. I. Merson et al. 2013) derived with the same method for COSMOS2020. On the other hand, the y-axis denotes the 3D spherical FoF fraction, taking into account a physical distance of 10 Mpc in the same mock data. They exhibit a general correlation within the 95% prediction level. The Pearson correlation coefficient is ρ and p-value p. The best-fit linear regression line is shown as a dashed line.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The QF as a function of the FoF fraction for the total 68 galaxy clusters found in the COSMOS field. The color code denotes the redshift of a given cluster. The gray dashed line is plotted as the median QF at a given FoF fraction with a 1σ confidence level (gray shade).
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The median QF in stellar mass bins of member galaxies in the TNG300 simulation. The QFs of isolated clusters are nearly identical to those in connected clusters over the entire stellar mass bin and regardless of the halo mass. For comparison, the observational data are shown in gray symbols, where the meanings of the points are the same as those in Figure 9.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The comparison of concentration parameters and QFs in connected (the open blue triangles) and isolated clusters (the filled red stars). No notable difference for c is found between the isolated and connected clusters.
Paper: Test of Cosmic Web-feeding Model for Star Formation in Galaxy Clusters in the COSMOS Field
Authors: Eunhee Ko, 은희 고, Myungshin Im, Seong-Kook Lee, Clotilde Laigle
Figure caption: The median QF as a function of the FoF fraction in the TNG300 simulation. The concentration parameter c fitted from the NFW profile (J. F. Navarro et al. 1997) is obtained from D. Anbajagane et al. (2022).
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Time evolution of the hot spots. The hot spots are split into four different quadrants (northeast (NE), northwest (NW), southeast (SE), and southwest (SW)) based on their position angles (PAs). Upper panels: time evolution of the radial distances of the different spots. The distances are inclination corrected and measured from the center of SN 1987A reported by D. Alp et al. (2018). The solid lines represent the best fits for the data after the emergence of the different spots used for the velocity estimations. Lower panels: flux evolution of the individual hot spots in the R band. The gray band represents the epochs of the WFPC2 measurements significantly affected by the CTE loss. To compensate for this, the fluxes of these measurements were multiplied by a factor of 1.25. The solid lines give the exponentially modified Gaussian best fits to the data after the emergence of the different spots.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Left panel: ACS/F625W image from 7226 days after the explosion (2006 December 6) showing all the identified hot spots in the ER as dots. The numbering of the spots is done anticlockwise from the north. Spot 5 is the one spot detected from the residual image at the second iteration. The center of the ER is marked by a black cross. The FOV is 2.″10 × 1.″73. Right panel: WFC3/F625W residual image from 10,698 days (2016 June 8) after the subtraction of all 26 fitted spots from the original image. The black dots represent the centroids of the 26 hot spots while the black crosses correspond to the three additional spots detected at the second iteration that were not included in our analysis. Red means brighter. Note the additional emission in the west, which becomes increasingly brighter in all residual images after 2015. The FOV is 2.″30 × 2.″13.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Time evolution of spot 2. The upper panels display the region of spot 2 (as defined in Figure 2) for all observations. The cross marker indicates the best-fit centroid of the detected source in that region, while the dashed ellipses showcase the orientation as well as the major and minor FWHM of the spot. The FOV of the panels is 350 × 375 mas2. In the lower panel, the radial distance of the detected source from the center of SN 1987A is depicted over time. Initially, the algorithm identifies and fits a source at the outer edge of the ER. Over time, as the blast wave encounters the ER, emission from the inner part of the ER dominates, causing a drop in the radial distance. Eventually, a minimum is reached around the year 1999, which we identify as the activation time of the spot. Subsequently, the radial distance increases systematically. The same general behavior is observed for the other spots.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Left panels: velocity distributions of the spots based on their models; straight and piecewise lines with breaks. The initial velocities are plotted separately from the subsequent ones to showcase that the spots are slowing down as time passes. Right upper panel: histograms of the flux peak times, estimated by the exponentially modified Gaussians. The histogram includes both the flux peak distribution of all spots and those that change velocity at least once. Right lower panel: the total distribution of all break times.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Scatterplot demonstrating the relationship between the time of maximum flux and the instances when the hot spots undergo velocity changes. The data set exhibits a Spearman correlation coefficient of 0.47 (p = 0.06), indicating a moderate positive correlation between the variables with marginal statistical significance.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: All HST R-band images used in the study, ranging from 1994 to 2022. The color scale is logarithmic, with the maximum set to the brightest hot spot in 2009 December to showcase the evolution of the ER. The field of view (FOV) of each image is 2.″30 × 2.″15. The spot in the southwest at approximately 5 o’clock is a star. We refer the reader to J. Larsson et al. (2019) and S. Rosu et al. (2024) for versions of these images that have color scales set to highlight the ejecta inside the ER.
Paper: Tracing the Propagation of Shocks in the Equatorial Ring of SN 1987A over Decades with the Hubble Space Telescope
Authors: Christos Tegkelidis, Josefin Larsson, Claes Fransson
Figure caption: Illustration of the number of breaks and velocities of the spots across the ER. The spots are color coded by their velocities, with the final velocity shown for cases where a velocity change occurred.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Comparison of the +31 day MODS spectrum with the 0.4 Z ⊙ (blue) and 0.1 Z ⊙ (red) model spectra from L. Dessart et al. (2013) at the same phase. Spectra are aligned to the Hβ blueshift of SN 2023ufx to ease visual comparisons. Important spectral features are marked.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Evolution of the [O I] λ5577 and [O I] λ6300 emission lines at ≈65–130 days after explosion. Blue dashed lines show the average velocity shift of each line, v 5577 ≈ −3300 km s−1 and v 6300 ≈ −3000 km s−1. The [O I] λ5577 line is twice as broad (≈2600 km s−1) compared to the [O I] λ6300 emission (≈1300 km s−1). Red arrows denote potential high-velocity features.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Normalized evolution of the Hα emission complex spanning ≈65–105 days after explosion. Phases for each spectrum are provided in the upper-left corner. [O I] appears at the onset of the radioactive-decay phase and strengthens with time. A redshifted Hα component appears in the last KCWI high-resolution spectrum—a comparison to the NIR spectra in Figure 13 confirms that this feature is not due to low-velocity He I λ6678. Labels along the top axis give velocities in 103 km s−1 for Hα (gray) and [O I] (red).
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: Comparing the high-quality +98 day spectrum to other SNe II in the literature. Each spectrum is aligned to Fe II λ5169 with the velocity offset given in each label. SN 2023ufx exhibits strong H absorption, weak Fe II features, and the blend of singly ionized metals from ≈4100 to 4500 Å is absent.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: NIR spectra of SN 2023ufx from SpeX (+51 days and ≈+115 days, black) shown alongside contemporaneous optical spectra from SNIFS (+48 days, purple) and MODS (+98 days, red). The Pα, Pβ, Pγ, and He I 1.083 μm features are marked with vertical colored lines. Regions with significant telluric absorption are shaded gray.
Paper: The Extremely Metal-poor SN 2023ufx: A Local Analog to High-redshift Type II Supernovae
Authors: Michael A. Tucker, Jason Hinkle, Charlotte R. Angus, Katie Auchettl, Willem B. Hoogendam, Benjamin Shappee, Christopher S. Kochanek, Chris Ashall, Thomas de Boer, Kenneth C. Chambers, Dhvanil D. Desai, Aaron Do, Michael D. Fulton, Hua Gao, Joanna Herman, Mark Huber, Chris Lidman, Chien-Cheng Lin, Thomas B. Lowe, Eugene A. Magnier, Bailey Martin, Paloma Mínguez, Matt Nicholl, Miika Pursiainen, S. J. Smartt, Ken W. Smith, Shubham Srivastav, Brad E. Tucker, Richard J. Wainscoat
Figure caption: The galaxy mass–metallicity plane discussed in Section 6.1. We compare the host galaxy of SN 2023ufx (gold star) to SDSS (gray points, D. J. Eisenstein et al. 2011), local dwarfs (dark blue points, D. A. Berg et al. 2012; T. Hsyu et al. 2018), SN II hosts (light blue points, P. L. Kelly & R. P. Kirshner 2012; C. P. Gutiérrez et al. 2018; K. Taggart & D. A. Perley 2021), and high-redshift galaxies from JWST (M. Curti et al. 2023; K. E. Heintz et al. 2023; K. Nakajima et al. 2023; T. Morishita et al. 2024) with the redshift given by the red color bar.