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Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions of the new coronae recognized in this work compared with those already known in the literature. With the exception of Oh 51, Platais 3, Oh 59, and Platais 9, most open clusters near the Sun lie in two distinct planes in Z, centered near Z ≈ −25 pc and Z ≈ 90 pc. The newly discovered corona around the 90 Myr old Volans–Carina association is the second closest known corona discovered so far, after that of the 680 Myr old Hyades association, and presents a unique opportunity for the search and characterization of its substellar members. Parts of the coronae shown here appear to be distributed along the line of sight, which is likely an artifact due to non-negligible parallax measurement errors. As shown by Meingast et al. (2021), a proper spatial deconvolution of these measurement errors shows coronae that are flat in the Z-direction and not preferentially aligned along the line of sight, but distributed along a spatial axis in the XY-plane that is unique to each open cluster. The contracted figure tags correspond to the following associations: PL9: Platais 9; ALES9: Alessi 9; PRA: Praesepe; VCA: Volans–Carina association; CBER: Coma Ber; HYA: Hyades; APER: α Persei; and PL3: Platais 3.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 216 and various subgroups associated with the Taurus–Auriga star-forming region (Liu et al. 2021; Kerr et al. 2021). The subgroup corresponding to μ Tau (Greater Taurus Subgroup 1 of Kerr et al. 2021) is not shown, and the subgroups corresponding to the 118 Tau association (Greater Taurus Subgroup 6 of Kerr et al. 2021, and Group 11 of Liu et al. 2021) and the 32 Ori association (Greater Taurus Subgroup 7 of Kerr et al. 2021) are with separate symbols. Crius 216 includes members of both the 118 Tau and 32 Ori associations, and they have UVW velocities in the vicinity of other Taurus subgroups, consistent with the hypothesis that they represent contiguous star formation events related with the larger complex of Taurus–Auriga members.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius groups that we have identified as putative extensions of generally more distant, known associations. Groups that are significantly extended on the sky will show large variations in observed tangential motions, causing clustering algorithms to recover them less efficiently unless they work in 3D UVW-space directly. Theia 1005 may be much more spatially extended than previously recognized in the XY-plane (top-row panels). Both Crius 151, Crius 205, and Crius 207 (bottom-row panels) were all associated with Theia 677 of Kounkel & Covey (2019), indicating that Theia 677 may be composed of distinct populations, the largest fraction of which likely corresponds to Crius 205 and Crius 207. These latter two appear as a potentially coeval population with a slightly bimodal density in XYZUVW-space, whereas Crius 151 shows significantly different kinematics and may therefore correspond to a distinct population that contaminated Theia 677 in part.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius groups that we have identified as putative extensions of generally more distant, known associations. Theia 310 of Kounkel & Covey (2019), in the top-row panels, may be spatially more extended than previously recognized along our line of sight, reaching within 100 pc of the Sun. The gap at 200 pc may be due to a low recovery rate by Kounkel & Covey (2019) caused by projection effects (the larger parallax correlates with larger tangential motions), and a low recovery rate in our study due to the lack of radial velocity measurements in Gaia DR2 at these farther distances. A similar structure is observed for Crius 227 and Theia 209, although the gap in members is located at closer distances (≈ 80 pc), and the putative spatial extension reaches well within the solar neighborhood down to 19 pc from the Sun, making this ensemble particularly interesting for the study of exoplanets and substellar objects.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Spread in properties as a function of distance for the new Crius candidate coeval associations presented here (red, filled circles), the other Crius groups that we have rejected based on various quality cuts (gray, open circles), and the Theia groups of Kounkel & Covey (2019). We show the median absolute deviations (MAD) instead of standard deviations to avoid the exaggerated impact of outliers due to low-quality measurements. These distributions outline how the large spread of sky coordinates at nearby distances can drive a larger spread in tangential velocities. Crius groups show much smaller UVW spreads compared with average Theia groups, as described in Section 3.6. The spreads in the Z-coordinate of Crius groups are comparable to those of the Theia groups, as should be expected.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 221, which likely corresponds to the front-facing tidal dissipation tail (or “corona”) of the 90 Myr old Volans–Carina association. Stars with full 3D UVW kinematics consistent with the core members of Volans–Carina within 3 km s−1 are indicated with distinct symbols; other stars will need heliocentric radial velocity measurements for their membership to be fully confirmed. This young structure that reaches within 22 pc of the Sun will be a valuable laboratory to study young exoplanets such as TOI–1224 b as well as substellar objects.
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius 226, which likely correspond to a corona around Group 59 of Oh et al. (2017). Theia 209 of Kounkel & Covey (2019) seems associated with the near side of Crius 226, and a small fraction of Theia 133 seems associated with its far side; however, Theia 133 also includes a much larger population of stars associated with the α Persei open cluster and its corona, the kinematics of which are discrepant with Crius 226 and Group 59 of Oh et al. (2017).
Paper: New Coronae and Stellar Associations Revealed by a Clustering Analysis of the Solar Neighborhood
Authors: Leslie Moranta, Jonathan Gagné, Dominic Couture, Jacqueline K. Faherty
Figure caption: Galactic positions and space velocities of Crius groups that we have identified as putative extensions of generally more distant, known associations. Crius 215 is a possible slight extension of Theia 600, perhaps corresponding to the forefront of the bimodal structure seen at larger distances.
Paper: Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: GSMFs estimated according to the designs in Table 1 using the Main sample (z  s  < 0.2, black), LOWZ (0.2 < z  s  < 0.4, red), and CMASS (0.5 < z  s  < 0.7, blue). The results from the Main sample are fitted by a double Schechter function shown in black line. The GAMA DR4 (Driver et al. 2022) measurements are provided for comparison and shown with purple diamonds. The GSFD (ρ * and Ω*) from the Main sample results is also given.
Paper: Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Stellar mass–r band magnitude relations for GAMA DR4 galaxies k-corrected to z  s  = 0.075, 0.1, 0.15, and 0.2. Galaxies are weighted by ﹩1/{V}_{\max }﹩. Red lines with dots show the 95% completeness limits C 95(M *) varying with the stellar mass at each redshifts. Gray dashed lines show the stellar mass limits for DECLaS with an r-band depth of 23.15 mag.
Paper: Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: The r − z vs. z − W1 color–color diagram for sources with z < 22.0 from DECaLS color-coded according to their photometric redshift (Zhou et al. 2021). Dashed line is the nonstellar cut adopted in DESI LRG target selection (Zhou et al. 2020) and solid lines are the cuts adopted in this work.
Paper: Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Comparing ﹩{ \mathcal A }/{\bar{n}}_{2}﹩ (lines) with w p (dots) for the Main sample. Each panel is for the same mass bin of pop2. Different colors are for different mass bins of pop1, and results are multiplied by 0.25, 0.5, 1, 2, and 4 for better illustration.
Paper: Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Comparisons of the GSMFs from PAC (red) and DECaLS photoz (blue; Zhou et al. 2021) at the massive ends for the LOWZ (left; 0.2 < z  p  < 0.4) and CMASS (right; 0.5 < z  p  < 0.7) redshift ranges.
Paper: Photometric Objects Around Cosmic Webs (PAC) Delineated in a Spectroscopic Survey. III. Accurate Measurement of Galaxy Stellar Mass Function with the Aid of Cosmological Redshift Surveys
Authors: Kun Xu, Y. P. Jing, Hongyu Gao
Figure caption: Left: stellar mass distributions for the Main, LOWZ and CMASS spectroscopic samples. Right: cumulative distribution function of the rband 10σ PSF depth for DECaLS.
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Upper and middle panels: core nuclear burning stages of massive stars with M = 12–80 M ⊙ as a function of time before collapse. Solid and dotted lines represent nonrotating and rotating stars with Ω = 0.5, as described in Shiode & Quataert (2014), respectively. Lower panel: amount of mass lost plotted against the location of the thick CSM for a subset of SNe in Figure 12 and follows the same color scheme. The x-axis of this plot maps into the x-axes of the middle and upper panels for an assumed wind speed of 10 km s−1 (top panel) or 1000 km s−1 (middle panel). Vertical black solid lines emphasize the location of the CSM material for SN 2014C. For the CSM mass of SN 2014C, we use an upper limit of f = 1 and a lower limit of f = 0.1. Additionally, we show the boundaries for which three wave-driven mass-loss episodes occurred in simulations. The magenta dotted–dashed line represents a Wu & Fuller (2021) model, and the gray dotted and dashed lines represent an H-rich and H-poor model from Leung et al. (2021b). Details of the model are described in Section 4.2.
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Side view cartoon depiction of the geometry around SN 2014C. The CSM is contained within the equatorial plane, beginning at a radius R  i  ∼ 2.2 × 1016 cm, which the FS achieved within 130 days post-explosion. Prior to 130 days, the FS was mostly spherical. Upon striking the equatorial CSM, that portion of the FS slowed down from ∼104 to ∼4 × 103 km s−1. This interaction of FS and CSM generates the observed X-rays, while the FS that was only slightly decelerated by a significantly lower-density medium at ∼104 km s−1 generates the observed radio emission. As the FS is only impeded in the equatorial plane, the radio emission creates an hourglass shape, which is consistent with the spherical symmetry found by Bietenholz et al. (2021b). A similar geometry has been invoked by Milisavljevic et al. (2015) and, more recently, by Thomas et al. (2022) for the specific case of SN 2014C, and also observationally for other SNe (e.g., Smith et al. 2015; Andrews & Smith 2018; Brennan et al. 2022a) and theoretically in hydrodynamical simulations (e.g., Kurfürst & Krtička 2019).
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Radial location (or extension) of the regions of high-density material for different types of SNe that showed evidence for CSM interaction at some point during their evolution. Type IIn SNe are included only in Tables 7 and 8 due to assumptions and uncertainties in their properties. This figure uses the same color scheme as Figures 11 and 13 (the legend also reflects the order that categories appear). Circles represent when the data includes a lower limit.
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Density profile of the CSM assuming solar chemical composition, as derived from NHint(t) (red triangles) and EM(t) (blue squares) following the assumptions stated in Section 3.3. We assume f = 1, ΔR = 0.1R(t), μ  e  = 1.25, and μ  I  = 1.15 in these calculations. Black dashed lines: wind-density profiles for a range of mass-loss rates ﹩\dot{M}﹩, i.e., (﹩{\rho }_{\mathrm{CSM}}=\dot{M}/(4\pi {v}_{w}{R}^{2})﹩) for ﹩\mathrm{log}(\dot{M}/{M}_{\odot }{\mathrm{yr}}^{-1})=[-2,-1.5,-1,-0.5,0]﹩ with an assumed wind speed of v  w  = 1000 km s−1. Due to a small change in NHint between observations for ∼7 × 1016 cm, the point is an upper limit as the error bars are approximately equal to the density measurement. Fitting with a power law, the density profile is best fit with ρ CSM ∝ R −2.42±0.17 and R −1.50±0.01, derived from NH(t) and EM(t), respectively. Both profiles are inconsistent with a wind profile, albeit with an extreme mass-loss rate. We note that the plotted error bars reflect statistical uncertainties only.
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: A comparison of the time frames of interaction using the same color scheme as in Figures 12 and 13 (the legend also reflects the order that categories appear). Most points are lower limits, as interaction was still ongoing as of the latest observation when the transient faded below the threshold of detection. Uncertainties in interaction onset are dominated by the time between consecutive observations. Type IIn SNe are included only in Tables 7 and 8 due to assumptions and uncertainties in their properties. Circles represent when the data include a lower limit.
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Incremental mass added between observations (left) and total mass (right) based on NHint(t) (red triangles) and EM(t) (blue squares). The NHint(t) masses are calculated via Equation (10) using radii from X-ray emission, while the EM(t) masses are calculated using Equations (5) and (6) under an assumption that shell thickness is 0.1R. Importantly, each measurement of accumulated mass from NHint(t) requires a following observation; hence, there is one fewer data point compared to the EM(t). The nonsolid lines represent a filling factor of 0.1 applied to each method, as estimated by line emission in Milisavljevic et al. (2015). We note that the plotted error bars reflect statistical uncertainties only (statistical uncertainty of EM(t) is smaller than the squares).
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Evolution of the Fe line emission (blue) and total emission (green, rescaled by 10−1) with time to show similarities in overall behavior. The Fe line emission is consistent with no change until δ t ≈ 850 days. The line emission starts to decay at t > 1000 days along with the X-ray continuum of Figure 5. The equivalent width of the Fe line emission remains roughly constant with time, suggesting a physical connection between the Fe line emission and the continuum emission.
Paper: Seven Years of Coordinated Chandra–NuSTAR Observations of SN 2014C Unfold the Extreme Mass-loss History of Its Stellar Progenitor
Authors: Daniel Brethauer, Raffaella Margutti, Dan Milisavljevic, Michael F. Bietenholz, Ryan Chornock, Deanne L. Coppejans, Fabio De Colle, Aprajita Hajela, Giacomo Terreran, Felipe Vargas, Lindsay DeMarchi, Chelsea Harris, Wynn V. Jacobson-Galán, Atish Kamble, Daniel Patnaude, Michael C. Stroh
Figure caption: Inferred temporal evolution of the radius of the shockwave that dominates the radio emission detected by VLBI (red triangles, Equation (4) from Bietenholz et al. 2021b), and the inferred radius of the X-ray emitting material (blue squares, Section 3.2) calculated using the shock velocity inferred from Equation (3). The thick, dotted, and dotted–dashed gray lines are the power-law evolution of the radius R ∝ t  n  with n = 0.8, n = 0.7, and n = 0.6, respectively, to guide the eye.
Paper: Experimental Determination of the Dissociative Recombination Rate Coefficient for Rotationally Cold CH+ and Its Implications for Diffuse Cloud Chemistry
Authors: Daniel Paul, Manfred Grieser, Florian Grussie, Robert von Hahn, Leonard W. Isberner, Ábel Kálosi, Claude Krantz, Holger Kreckel, Damian Müll, David A. Neufeld, Daniel W. Savin, Stefan Schippers, Patrick Wilhelm, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: CH+ DR kinetic temperature rate coefficient and its relevance for the CH+ destruction in diffuse interstellar clouds. (a) The thick solid line shows the experimentally determined J = 0 kinetic temperature rate coefficient of this work. The one-sigma error band in gray represents the quadrature sum of all systematic uncertainties. The dashed lines indicate rate coefficients from the astrochemistry databases UMIST (McElroy et al. 2013, upper line) and KIDA (Wakelam et al. 2012, lower line). The calculated J = 0 rate coefficient of Mezei et al. (2019) is drawn as dotted line. (b) Diffuse cloud parameter ranges where DR is the dominant CH+ destruction process for a standard electron fraction (χ e = 1.6 × 10−4) and for enhanced values of χ e as given. The relevant range is to the left of each labeled curve. One-sigma error bars for ﹩{f}_{{{\rm{H}}}_{2}}=1﹩ and ﹩{f}_{{{\rm{H}}}_{2}}=0﹩ are shown at the top and bottom of the figure, respectively. They were calculated from the combined systematic uncertainties for the rate coefficients α H (∼50%, Plasil et al. 2011), ﹩{\alpha }_{{{\rm{H}}}_{2}}﹩ (∼20%, Gerlich et al. 2011), and ﹩{\alpha }_{J=0}^{{\rm{k}}}﹩ (∼20%, this work).
Paper: Experimental Determination of the Dissociative Recombination Rate Coefficient for Rotationally Cold CH+ and Its Implications for Diffuse Cloud Chemistry
Authors: Daniel Paul, Manfred Grieser, Florian Grussie, Robert von Hahn, Leonard W. Isberner, Ábel Kálosi, Claude Krantz, Holger Kreckel, Damian Müll, David A. Neufeld, Daniel W. Savin, Stefan Schippers, Patrick Wilhelm, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: (a) Schematic of the CSR experimental setup for DR measurements of CH+ and probing of its internal-level populations. See text for details. (b) Measured relative J-level populations in the CSR for storage times of 60–80 s with statistical one-sigma error bars. (c) Relative J-level populations predicted in TSR for a thermal equilibrium at T = 300 K.
Paper: Experimental Determination of the Dissociative Recombination Rate Coefficient for Rotationally Cold CH+ and Its Implications for Diffuse Cloud Chemistry
Authors: Daniel Paul, Manfred Grieser, Florian Grussie, Robert von Hahn, Leonard W. Isberner, Ábel Kálosi, Claude Krantz, Holger Kreckel, Damian Müll, David A. Neufeld, Daniel W. Savin, Stefan Schippers, Patrick Wilhelm, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Merged-beams DR rate coefficient (blue line) for the CH+ ground state X 1Σ+(v = 0, J = 0) with the statistical one-sigma uncertainties (blue shaded area). The one-sigma uncertainty of the absolute scale is ±13%. The room-temperature TSR results of Amitay et al. (1996), which have a ±50% absolute scaling systematic uncertainty, are shown by the gray squares. The symbols and lines on top of the figure indicate the FWHM energy resolution ΔE of the CSR and TSR measurements. The divergence of the CSR from the TSR data for E d ≳ 10 eV is due to contribution from dissociative excitation (see text). The data behind the TSR and CSR graphs are both available. The latter are part of Figure 5(b).(The data used to create this figure are available.)