adsabs/AstroCLIMB huggingface dataset:
Paper: Properties of Host Galaxies of Submillimeter Sources as Revealed by JWST Early Release Observations in SMACS J0723.3–7327
Authors: Cheng Cheng, Haojing Yan, Jia-Sheng Huang, Christopher N. A. Willmer, Zhiyuan Ma, Gustavo Orellana-González
Figure caption: The evolution of the 1.1 mm to Ks observed flux ratio as a function of redshift. We show the submillimeter galaxies (SMGs) from Gómez-Guijarro et al. (2022) (ALMA-GOODS 2.0). The expected trends for a starburst galaxy (Arp 220, dotted red line), a typical star-forming galaxy (dotted–dashed blue line), and a QSO (dashed green line). Both ID2 and ID3 follow the trend of Arp 220 well, but ID1 shows a flux ratio that is too high, suggesting a high-z nature of this target.
Paper: Properties of Host Galaxies of Submillimeter Sources as Revealed by JWST Early Release Observations in SMACS J0723.3–7327
Authors: Cheng Cheng, Haojing Yan, Jia-Sheng Huang, Christopher N. A. Willmer, Zhiyuan Ma, Gustavo Orellana-González
Figure caption: The V − J vs. U − V diagram of our sample. We show the CANDELS (Grogin et al. 2011; Koekemoer et al. 2011) sample at redshifts 1 < z < 2.5 as a comparison. The solid lines are adopted from Fang et al. (2018) to separate quiescent from star-forming galaxies.
Paper: The Unmixed Debris of Gaia-Sausage/Enceladus in the Form of a Pair of Halo Stellar Overdensities
Authors: Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Silvia Rossi, Anna B. A. Queiroz, Rafael M. Santucci, Angeles Pérez-Villegas, Cristina Chiappini
Figure caption: Spatial projection in Galactic coordinates of the SEGUE sample selection of the stellar overdensities (left). Distribution of the sample of stars from SEGUE in the X GC–Y GC (top right) and X GC–Z GC projections (bottom right). The HAC-S, HAC-N, and VOD are represented by orange squares, violet circles, and blue diamonds, respectively. The rings are concentric with the center of the Galaxy.
Paper: Observation of a Magnetic Switchback in the Solar Corona
Authors: Daniele Telloni, Gary P. Zank, Marco Stangalini, Cooper Downs, Haoming Liang, Masaru Nakanotani, Vincenzo Andretta, Ester Antonucci, Luca Sorriso-Valvo, Laxman Adhikari, Lingling Zhao, Raffaele Marino, Roberto Susino, Catia Grimani, Michele Fabi, Raffaella D'Amicis, Denise Perrone, Roberto Bruno, Francesco Carbone, Salvatore Mancuso, Marco Romoli, Vania Da Deppo, Silvano Fineschi, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Luca Teriaca, Federica Frassati, Giovanna Jerse, Federico Landini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Ruggero Biondo, Aleksandr Burtovoi, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Yara De Leo, Marina Giarrusso, Alessandro Liberatore, David Berghmans, Frédéric Auchère, Regina Aznar Cuadrado, Lakshmi P. Chitta, Louise Harra, Emil Kraaikamp, David M. Long, Sudip Mandal, Susanna Parenti, Gabriel Pelouze, Hardi Peter, Luciano Rodriguez, Udo Schühle, Conrad Schwanitz, Phil J. Smith, Cis Verbeeck, Andrei N. Zhukov
Figure caption: (a) Composite of the Metis-observed tB image of the solar corona within 3.5 R ⊙ FOV (blue) and the EUI image of the ultraviolet emission (yellow) as viewed from the SO vantage point on 2022 March 25 at 20:39 UT. (b) Same as in panel (a), but with the Metis observations radially filtered with the SiRGraF algorithm. (c) Zoom-in of panel (b); overlaid is the rectangular ROI where the time–distance analysis on the S-shaped structure was performed, and a white square indicating the loop system associated with AR 12972. (d) Coronal velocity map in the same FOV as in panel (c); the white dotted line marks the latitude relative to the S-shaped feature.
Paper: Observation of a Magnetic Switchback in the Solar Corona
Authors: Daniele Telloni, Gary P. Zank, Marco Stangalini, Cooper Downs, Haoming Liang, Masaru Nakanotani, Vincenzo Andretta, Ester Antonucci, Luca Sorriso-Valvo, Laxman Adhikari, Lingling Zhao, Raffaele Marino, Roberto Susino, Catia Grimani, Michele Fabi, Raffaella D'Amicis, Denise Perrone, Roberto Bruno, Francesco Carbone, Salvatore Mancuso, Marco Romoli, Vania Da Deppo, Silvano Fineschi, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Luca Teriaca, Federica Frassati, Giovanna Jerse, Federico Landini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Ruggero Biondo, Aleksandr Burtovoi, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Yara De Leo, Marina Giarrusso, Alessandro Liberatore, David Berghmans, Frédéric Auchère, Regina Aznar Cuadrado, Lakshmi P. Chitta, Louise Harra, Emil Kraaikamp, David M. Long, Sudip Mandal, Susanna Parenti, Gabriel Pelouze, Hardi Peter, Luciano Rodriguez, Udo Schühle, Conrad Schwanitz, Phil J. Smith, Cis Verbeeck, Andrei N. Zhukov
Figure caption: Horizontally-oriented frames of the ROI overlaid in Figure 1(c) every 400 s starting at 20:11 UT on 2022 March 25 (top panel). The upper x-axis indicates the distance from the Sun. The slope of the displayed red dashed line, connecting the radial positions of the main ripple front over time, indicates an almost constant propagation speed of ∼80 km s−1.
Paper: Observation of a Magnetic Switchback in the Solar Corona
Authors: Daniele Telloni, Gary P. Zank, Marco Stangalini, Cooper Downs, Haoming Liang, Masaru Nakanotani, Vincenzo Andretta, Ester Antonucci, Luca Sorriso-Valvo, Laxman Adhikari, Lingling Zhao, Raffaele Marino, Roberto Susino, Catia Grimani, Michele Fabi, Raffaella D'Amicis, Denise Perrone, Roberto Bruno, Francesco Carbone, Salvatore Mancuso, Marco Romoli, Vania Da Deppo, Silvano Fineschi, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Luca Teriaca, Federica Frassati, Giovanna Jerse, Federico Landini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Ruggero Biondo, Aleksandr Burtovoi, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Yara De Leo, Marina Giarrusso, Alessandro Liberatore, David Berghmans, Frédéric Auchère, Regina Aznar Cuadrado, Lakshmi P. Chitta, Louise Harra, Emil Kraaikamp, David M. Long, Sudip Mandal, Susanna Parenti, Gabriel Pelouze, Hardi Peter, Luciano Rodriguez, Udo Schühle, Conrad Schwanitz, Phil J. Smith, Cis Verbeeck, Andrei N. Zhukov
Figure caption: Modeled magnetic field lines (a) and rendered squashing factor Q (b) from the SO point of view on 2022 March 25. Carrington maps of ﹩\mathrm{log}Q﹩ at 3 R ⊙ (c), photospheric radial magnetic field (d), and open-field regions on the Sun’s surface (e). The Carrington longitude of the eastern Metis FOV on 2022 March 25 at 20:39 UT and the heliographic latitude of the observed S-shaped structure are marked by the black vertical and horizontal dashed lines, respectively. AR 12972 and the associated open flux are indicated by a green arrow. The latter maps to the PS curtain and the HCS (as indicated by color-coded arrows) in several places in latitude and longitude, forming a null-point signature (denoted by the orange arrow).
Paper: Observation of a Magnetic Switchback in the Solar Corona
Authors: Daniele Telloni, Gary P. Zank, Marco Stangalini, Cooper Downs, Haoming Liang, Masaru Nakanotani, Vincenzo Andretta, Ester Antonucci, Luca Sorriso-Valvo, Laxman Adhikari, Lingling Zhao, Raffaele Marino, Roberto Susino, Catia Grimani, Michele Fabi, Raffaella D'Amicis, Denise Perrone, Roberto Bruno, Francesco Carbone, Salvatore Mancuso, Marco Romoli, Vania Da Deppo, Silvano Fineschi, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Luca Teriaca, Federica Frassati, Giovanna Jerse, Federico Landini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Ruggero Biondo, Aleksandr Burtovoi, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Yara De Leo, Marina Giarrusso, Alessandro Liberatore, David Berghmans, Frédéric Auchère, Regina Aznar Cuadrado, Lakshmi P. Chitta, Louise Harra, Emil Kraaikamp, David M. Long, Sudip Mandal, Susanna Parenti, Gabriel Pelouze, Hardi Peter, Luciano Rodriguez, Udo Schühle, Conrad Schwanitz, Phil J. Smith, Cis Verbeeck, Andrei N. Zhukov
Figure caption: Power spectral density of velocity fluctuations transverse to the main ripple propagation direction. A characteristic 12 mHz frequency emerges clearly.
Paper: The Planetary Nebula in the 500 Myr Old Open Cluster M37
Authors: Vasiliki Fragkou, Quentin A. Parker, Albert A. Zijlstra, Roberto Vázquez, Laurence Sabin, Jackeline Suzett Rechy-Garcia
Figure caption: Left panel: a plot from the known sample of cluster white dwarfs for the latest IFMR estimates and semiempirical “PARSEC” fit (Cummings et al. 2018) together with our estimated point for PN IPHAS J055226.2+323724 plotted as a red circle. The other two points from known open-cluster PNe are plotted as a yellow circle (PHR 1315-6555 Fragkou et al. 2019b and Parker et al. 2011) and a green circle (BMP J1613-5406 - Fragkou et al. 2019a). The errors attached to our point reflect the errors in the adopted cluster parameters and the spread of the estimated central star magnitudes. Right panel: the initial–final mass relation of Marigo et al. (2020) with the two cluster PNe within this mass range
Paper: The Planetary Nebula in the 500 Myr Old Open Cluster M37
Authors: Vasiliki Fragkou, Quentin A. Parker, Albert A. Zijlstra, Roberto Vázquez, Laurence Sabin, Jackeline Suzett Rechy-Garcia
Figure caption: Cluster Gaia DR3 CMD (B vs. B-R) diagram fitted with a Padova theoretical isochrone (Bressan et al. 2012; Marigo et al. 2013) for adopted cluster parameters (age = 470 ± 50 Myr, reddening E(B − V) = 0.26 ± 0.04, distance = 1.49 ± 0.13 kpc and metallicity [Fe/H] = 0.03 ± 0.28). The CSPN is indicated by the red filled symbol. Stars with >80% probability (Cantat-Gaudin et al. 2018) of being a cluster member, based on Gaia DR3 data, are plotted as green dots. The CMD includes all stars with pmRA = 0–4 and pmDec = −8 to −2 mas yr−1 (most probable cluster members based on mean proper motions) within 15′ from the cluster’s apparent center.
Paper: Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum
Authors: Michael Zevin, Daniel E. Holz
Figure caption: Evolution of merger product mass (M f, top row), dimensionless spin magnitude (χ f, middle row), and recoil kick velocity (V k, bottom row) of merger products that have proceeded through N merge mergers. The columns show the evolution of the three different pairing channels described in Section 2.2, with colors showing either the LVC (green) or IMF (orange) 1G populations. Colored bands contain 90% of systems, with lines showing representative randomly selected merger histories. At N merge = 0 we plot the mass and spin values for the primary component of the initial binary and do not show a value for the recoil kick velocity because the binary has yet to merge. Merger product masses grow exponentially in the NG+NG pairing scenario and the distribution of recoil kicks remains broad, whereas the mass growth flattens out in the intergenerational NG+1G and NG+ ≤ NG pairing scenarios, with the recoil kick distribution approaching 0 km s−1 as a function of N merge because the mass ratio of subsequent mergers enters the regime of q ≪ 1 in these pairing scenarios. Note that the range of N merge plotted on the horizontal axis varies between pairing methods.
Paper: Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum
Authors: Michael Zevin, Daniel E. Holz
Figure caption: Expected fraction of hierarchical BBH mergers with a source-frame total mass greater than 100 M ⊙ as a function of escape velocity for the three hierarchical merger pairing models. Green and orange markers denote the LVC and IMF 1G pairings, respectively, with marker styles denoting different assumptions for the total BH budget available for hierarchical assembly. The cyan shaded region marks the 90% credible interval of the posterior predictive distribution from the Power Law + Peak model; the lower end of this interval stretches below the vertical bounds of this figure. Markers for the IMF 1G population are artificially offset for readability. Points that lie on the horizontal axis indicate that f(M tot > 100M ⊙) < 10−5. Points that lie above the cyan shaded region overproduce massive BHs if hierarchical mergers exclusively account for the full BBH population; this is observed in most models where escape velocities are ≥300 km s−1. Reducing the BH budget available for hierarchical assembly only has a noticeable effect at values of ≲30.
Paper: Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum
Authors: Michael Zevin, Daniel E. Holz
Figure caption: Same as Figure 3, except with differing line styles showing the mass distribution for various assumptions regarding the model for delay times between subsequent mergers. Slightly extending the delay-time distribution to Δt = [10 Myr, 1 Gyr] has virtually no effect on the underlying mass distribution and pushes the detectable distribution to slightly higher masses due to more systems merging within the horizon of GW detectors. The long delay-time distribution of Δt = [100 Myr, 14 Gyr] pushes both the underlying and detectable hierarchical merger mass spectra to lower masses due to higher-generational merger products preferentially merging beyond the present day. Only the LVC 1G population model is shown for clarity.
Paper: Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum
Authors: Michael Zevin, Daniel E. Holz
Figure caption: Fraction of merger products retained as a function of the number of mergers in the hierarchical assembly process. Colored lines indicate various assumptions for escape velocities, and solid and dashed lines indicate the LVC and IMF 1G population, respectively. Retention fractions always decrease as a function of N merge in the NG+NG pairing scenario, whereas for escape velocities ≥200 km s−1 the retention fractions in the NG+1G pairing scenario asymptote to specific values as a function of N merge; once hierarchical merger products enter this regime, recoil kicks never eject them from their environment. Note that the range of N merge plotted on the horizontal axis varies between pairing methods.
Paper: Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum
Authors: Michael Zevin, Daniel E. Holz
Figure caption: Cumulative distributions for the underlying (left) and detectable (right) BBH merger mass distributions using the three pairing methods of hierarchical mergers (top, middle, and bottom). Solid lines use the LVC and dashed lines use the IMF 1G population model, with different colors denoting different escape velocities of the dynamical environment. Cyan bands represent constraints from existing data, showing the 90% credible region of the posterior predictive distribution inferred using the Power Law + Peak mass model in the LVC analysis of Abbott et al. (2021c). Across pairing scenarios and 1G population assumptions, hierarchical assembly in our models with escape velocities ≳300 km s−1 predict more high-mass mergers than the constraints by the LVC.
Paper: Avoiding a Cluster Catastrophe: Retention Efficiency and the Binary Black Hole Mass Spectrum
Authors: Michael Zevin, Daniel E. Holz
Figure caption: Same as Figure 3, except with differing line styles showing the mass distribution for various assumptions regarding the total budget of BHs available for mergers. Lowering the total BH budget available for hierarchical assembly naturally pushes the hierarchical merger mass spectra to lower masses as it truncates the hierarchical assembly after less repeated mergers, though this parameter has little impact on the mass spectrum so long as the BH budget is ≳30–100, depending on the pairing scenario. Only the LVC 1G population model is shown for clarity.
Paper: The Planetary Nebula in the 500 Myr Old Open Cluster M37
Authors: Vasiliki Fragkou, Quentin A. Parker, Albert A. Zijlstra, Roberto Vázquez, Laurence Sabin, Jackeline Suzett Rechy-Garcia
Figure caption: Figure 2(a) left panel: An enhanced 6.′5 × 6.′5 color-composite RGB image of PN IPHASX J055226.2+323724 from the IPHAS survey (Drew et al. 2005) that we confirm as a physical member of the Galactic open cluster M37. Red = Hα, Green = broad band red, and Blue = broad band “i”. The CSPN is circled in blue; Figure 2(b) right panel: 190 × 145″ RGB image created from SDSS with red = i, green = r and blue = g-band. These data clearly show the faint CSPN (arrowed) at the center. North is top, and east is to the left in both images.
Paper: The Planetary Nebula in the 500 Myr Old Open Cluster M37
Authors: Vasiliki Fragkou, Quentin A. Parker, Albert A. Zijlstra, Roberto Vázquez, Laurence Sabin, Jackeline Suzett Rechy-Garcia
Figure caption: A contrast-enhanced 30′ × 30′ quotient (Hα − r band) IPHAS (Drew et al. 2005) mosaic centered on the core of Galactic open cluster M 37 (NGC 2099). The low surface brightness bipolar PN (IPHASX J055226.2+323724) is encompassed by a red circle with a diameter of 445″ ± 10″ (the nebular major axis) while the blue circle indicates the full ∼30′ extent of the cluster. The PN is well within the cluster tidal radius with the blue CSPN at almost the precise geometric center of the PN. The CSPN is itself only ∼280″ from the published cluster center position.
Paper: The Planetary Nebula in the 500 Myr Old Open Cluster M37
Authors: Vasiliki Fragkou, Quentin A. Parker, Albert A. Zijlstra, Roberto Vázquez, Laurence Sabin, Jackeline Suzett Rechy-Garcia
Figure caption: Left panel: PN image with MEGARA IFU pointings indicated. Right panel: a combined 1D continuum subtracted example PN spectrum from 2022 March 4 for IFU pointings a, b, c, and d. The five visible PN emission lines are labeled.
Paper: Observation of Magnetic Reconnection in a Region of Strong Turbulence
Authors: R. E. Ergun, N. Pathak, M. E. Usanova, Y. Qi, T. Vo, J. L. Burch, S. J. Schwartz, R. B. Torbert, N. Ahmadi, F. D. Wilder, A. Chasipis, D. L. Newman, J. E. Stawarz, M. Hesse, D. L. Turner, D. Gershman
Figure caption: Near-EDR observations. The vertical dashed lines indicate (left) the current sheet and (right) the X-line retreating past MMS. Vectors are in LMN coordinates. (a)  B  at 128 samples s−1. (b)  V  Ion at 150 ms resolution. (c)  V  Elc at 30 ms resolution.  V  Elc is derived from integration of the electron distribution. (d)  E  at 8192 samples s−1. (e)  J  derived from ∇ ×  B /μ  o  at 128 samples s−1. The orange trace is ∇ ·  B /μ  o , which is a measure of the accuracy of  J . (f)  J  ·  E  at the MMS barycenter at 128 samples s−1. (g) MMS formation in LMN. (h) Plasma conditions and LMN values.
Paper: Observation of Magnetic Reconnection in a Region of Strong Turbulence
Authors: R. E. Ergun, N. Pathak, M. E. Usanova, Y. Qi, T. Vo, J. L. Burch, S. J. Schwartz, R. B. Torbert, N. Ahmadi, F. D. Wilder, A. Chasipis, D. L. Newman, J. E. Stawarz, M. Hesse, D. L. Turner, D. Gershman
Figure caption: (a), (b), and (c) B  L , B  M , and B  N  from the four MMS satellites.  B  shows higher fluctuations than observed in laminar magnetic reconnection. (d)–(i) The smoothed path of the MMS satellites with respect to the X-line constructed using the retreat velocity (200 km s−1 in L) and time delays in B  L  for N velocity over four segments. The values of B  L , B  M , E  N , J  L , J  M , and XLM  are represented by color. The shaded region marks a possible electromagnetic deflection of J  L . J  L , J  M , and XLM  are derived by integration of electron distributions from the MMS database; they are not the moments in the database.
Paper: Observation of Magnetic Reconnection in a Region of Strong Turbulence
Authors: R. E. Ergun, N. Pathak, M. E. Usanova, Y. Qi, T. Vo, J. L. Burch, S. J. Schwartz, R. B. Torbert, N. Ahmadi, F. D. Wilder, A. Chasipis, D. L. Newman, J. E. Stawarz, M. Hesse, D. L. Turner, D. Gershman
Figure caption: The electron distribution in the current sheet and in the jet as it emerges from the EDR (see Figure 4). (a) Off-diagonal stress is evident in the M–L plane. Crescent-shaped structures are visible. (b) The M–N plane shows the current sheet and (c) the L–N plane shows the electron jet. There is a large uncertainty inside the white circle due to spacecraft photoelectrons. (d) and (e) Electron V  L  and XLM  from MMS1, MMS2, and MMS3.
Paper: Observation of Magnetic Reconnection in a Region of Strong Turbulence
Authors: R. E. Ergun, N. Pathak, M. E. Usanova, Y. Qi, T. Vo, J. L. Burch, S. J. Schwartz, R. B. Torbert, N. Ahmadi, F. D. Wilder, A. Chasipis, D. L. Newman, J. E. Stawarz, M. Hesse, D. L. Turner, D. Gershman
Figure caption: (a) A cartoon of a retreating X-line and expanding region of turbulence. (b)  B  and  E  power spectral density. The low-frequency spectra are from the entire 30-minute turbulent period. The high-frequency spectra are from a ∼2 1/2 minute period when burst data are available. (c) A histogram of  J  ·  E  showing net particle energization.
Paper: The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A
Authors: Tanmoy Laskar, Alicia Rouco Escorial, Genevieve Schroeder, Wen-fai Fong, Edo Berger, Péter Veres, Shivani Bhandari, Jillian Rastinejad, Charles D. Kilpatrick, Aaron Tohuvavohu, Raffaella Margutti, Kate D. Alexander, James DeLaunay, Jamie A. Kennea, Anya Nugent, K. Paterson, Peter K. G. Williams
Figure caption: Left: theoretical 90 GHz light curves for 22 SGRBs (plus 211106A, magenta stars) with known redshift and published E K,iso and n 0 (lines, including collimation effects, where a jet break has been inferred). Six events have mm-band observations (colored points and lines). Empty triangles are mm-band upper limits for an additional five SGRBs with unknown physical parameters. Previous observations have failed to detect mm-band afterglows owing to a combination of insufficient sensitivity (pre-ALMA; horizontal dotted line) and incommensurate cadence (Section 5.3); however, 9/23 events (indicated by solid lines) would have been detected by ALMA in 30 minutes on source (horizontal dashed line). Right: n 0 vs. E K,iso for SGRB afterglows from Fong et al. (2015) divided into three redshift bins, with the median redshift and redshift range indicated in the upper-right corners. Events that have been observed in the mm band are indicated by colored circles and those with no measured redshifts are plotted as open circles at fiducial values of z = 0.5 or z = 1.0. The position of GRB 211106A is marked by the magenta star. The parameter space in each subplot is divided by lines at four different values of θ jet (values indicated in the rightmost subpanel), to the right of which the afterglow is expected to be detectable with ALMA for ≳2 days (Section 5.3).