adsabs/AstroCLIMB huggingface dataset:
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Disk-averaged CO intensity as a function of mid-IR intensity for integrated galaxies. CO (1–0) and CO (2–1) intensity (y-axis, top and bottom) as a function of 12 and 22 μm intensity derived from WISE photometry. There are about 800 and 350 galaxies in the CO (1–0) and CO (2–1) panels, respectively (see Table 1). All measurements are presented as averages within the stellar effective radius. Some of the aperture corrections dominate the size of the error bars, leading to a subset of CO (2–1) data with larger uncertainties. Black stars show integrated measurements for galaxies that have a resolved CO map. Colored points show the median I CO in bins of mid-IR intensity, with error bars indicating the 16%–84% range in the data. The light dotted lines in the background all have a slope of 1, indicating linear relations. The black line and shaded region show a power-law fit to the binned data and the rms of the residuals of individual data about that fit. The offset between mapped galaxies and the binned data in CO (1–0) likely reflects a sample bias (see Section 3.4).
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Sample of galaxies studied in star formation rate (SFR) vs. stellar mass (M ⋆) space. Each point corresponds to one of the galaxies that we study, with solid symbols indicating galaxies detected in both WISE3 and the relevant CO line for that panel. The top row shows the properties of galaxies with integrated measurements, while the bottom row highlights integrated measurements for galaxies with CO mapping. In each panel, we indicate the “main sequence” relation between SFR and M ⋆ from Leja et al. (2022) with a ±0.4 dex range. The black-and-white circles show the median and the corresponding error bars show the 16%–84% range of SFR at fixed M ⋆ for all galaxies detected in WISE3 and the CO line shown in that panel. Overall the integrated CO (1–0) and CO (2–1) sample and the mapping CO (2–1) data cover the star-forming main sequence, and we expect that they represent the overall z = 0 massive, star-forming galaxies well. The CO (1–0) mapping coverage is somewhat more restricted and slightly biased, a topic that we discuss in detail in Section 3.4. Low-mass dwarf galaxies and low SFR/M ⋆ early-type galaxies are not well covered by our sample. See Tables 1 and 2 for more information.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Index of power-law fits of I CO vs. I MIR for different band and line combinations. Each point shows the power-law index, m CO-IR, of a fit relating I CO to I MIR for one line-band combination. We plot results for galaxies, rings, and individual regions separately. The estimated methodological (systematic) error in m CO-IR is ±0.1; the formal errors are very small. The top axis shows the inverse of index, m IR-CO, which is the more common sense used to phrase star formation–gas scaling relations. Most results cluster relatively near a slope of ∼1. CO (2–1) systematically tends to yield a moderately steeper slope than CO (1–0) for the same mid-IR band. The 8 and 12 μm bands, which contain major PAH features, tend to yield steeper CO-to-IR slopes than the 22 and 24 μm bands, which capture mostly continuum emission.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Normalization of power-law fits of I CO vs. I MIR for different band and line combinations. As Figure 7 but now showing the normalization of the best-fit power-law relations for each line-band combination from Table 3. The black line marks the simple rule-of-thumb I CO ∼ 1 K km s−1 at I MIR ∼ 1 MJy sr−1. For CO (1–0) points we color our best estimates, which include a statistical correction to reflect possible biases in sample selection. However, we also show the original measurements in gray. Overall, we find fainter CO (2–1) compared to CO (1–0) at fixed I MIR and the CO-to-mid-IR ratio varies by band with the sense that I CO/I 12 μm > I CO/I 22 μm ∼ I CO/I 24 μm > I CO/I 8 μm.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Azimuthally averaged CO intensity as a function of mid-IR intensity at 12 and 22 μm from WISE for moderately resolved galaxies. As Figure 2 but now showing data for azimuthally averaged rings (radial profiles), within galaxies that have matched-resolution CO and mid-IR mapping (about 1000–1100 rings per panel detected in box axes depending on the bands; see Table 1). The light gray points show data with S/N < 5, and the binned medians are calculated including these data as well as data with I CO < 0, effectively stacking all available maps (about 160−330 limits per panel depending on the bands). For CO (1–0) the dotted line shows the expected relation applying a statistical correction (see Section 3.4) to adjust the resolved mapping sample to better reflect the integrated-galaxy sample.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Region-by-region averaged CO intensity as a function of mid-IR intensity at 12 and 22 μm from WISE for moderately resolved galaxies. As Figure 3 but now showing data for individual 17″ regions within galaxies that have matched-resolution CO and mid-IR mapping. As in Figure 3, the light gray points show data with S/N < 5, and the bins include these data as well as data with I CO < 0. Given the lower S/N of individual regions, including all data in the binned medians is key to avoid biasing the results. For CO (1–0) the dotted line shows the expected relation after applying the statistical correction to adjust the resolved mapping sample to better reflect the integrated-galaxy sample (Section 3.4).
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Region-by-region CO intensity as a function of mid-IR intensity at 8 and 24 μm from Spitzer for moderately resolved galaxies. As Figure 5 but now showing data for individual regions within galaxies that have targeted mid-IR mapping from Spitzer.
Paper: PHANGS–JWST First Results: A Global and Moderately Resolved View of Mid-infrared and CO Line Emission from Galaxies at the Start of the JWST Era
Authors: Adam K. Leroy, Alberto D. Bolatto, Karin Sandstrom, Erik Rosolowsky, Ashley. T. Barnes, F. Bigiel, Médéric Boquien, Jakob S. den Brok, Yixian Cao, Jérémy Chastenet, Mélanie Chevance, I-Da Chiang, 宜達 江, Ryan Chown, Dario Colombo, Sara L. Ellison, Eric Emsellem, Kathryn Grasha, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric W. Koch, Jaeyeon Kim, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Rebecca C. Levy, Lihwai Lin, Daizhong Liu, Sharon E. Meidt, Jérôme Pety, Miguel Querejeta, Mónica Rubio, Toshiki Saito, Samir Salim, Eva Schinnerer, Mattia C. Sormani, Jiayi Sun, David A. Thilker, Antonio Usero, Stuart N. Vogel, Elizabeth J. Watkins, Cory M. Whitcomb, Thomas G. Williams, Christine D. Wilson
Figure caption: Azimuthally averaged CO intensity as a function of mid-IR intensity at 8 and 24 μm from Spitzer for moderately resolved galaxies. As Figure 3 but now showing data for azimuthal averages within galaxies that have mid-IR mapping from Spitzer. The overall consistency with the WISE results is good.
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: Li abundances of pRC, sRC, and RGB giants as a function of stellar mass. Horizontal lines mark the first dredge-up theoretical upper limit of A(Li) = 1.8 dex for a giant with M = 1.5 M ⊙ and A(Li) = 3.2 dex for the super Li-rich giants. The error cross at the bottom right represents the mean errors in A(Li) and mass.
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: Shown are the sample giants of RC and RGB. In panel (a), 16,094 stars (red symbols) from Yu et al. (2018) are plotted with the entire Kepler sample as background. In panel (b), asteroseismically classified RGB and RC sample stars in this study are shown along with the sample giants from Vrard et al. (2016).
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: Determination of Li abundances for a few representative giants using spectrum synthesis around the Li 6707.8 Å resonance line.
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: Measurement of period spacing. The top-left panel is the PDS of RGB star KIC 8028908, and the right panel is the PDS of the RC star KIC 8540615. Oscillation modes of l = 0, 1, 2 are identified and marked in the figure. The bottom panel is a demonstration of the measurement of mixed-mode (l = 1) period spacing (ΔP). The red dotted horizontal line is the average value of the period spacing in each bottom panel.
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: The pRC and sRC giants in a luminosity and A(Li) plot superposed with MESA models of 1–5 M ⊙ giants. Note the many LRGs including SLRGs among pRCs and none among sRCs. Models show pRCs suffer severe depletion of Li during first dredge-up and also at the luminosity bump.
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: He-core mass and luminosity as a function of stellar mass for two metallicities for stars evolving from the main sequence to core helium burning (CHeB) phases.
Paper: Lithium Abundances in Giants as a Function of Stellar Mass: Evidence for He Flash as the Source of Li Enhancement in Low-mass Giants
Authors: Anohita Mallick, Raghubar Singh, Bacham E. Reddy
Figure caption: Average period spacing derived by us compared to values obtained by Vrard et al. (2016).
Paper: HAWC Detection of a TeV Halo Candidate Surrounding a Radio-quiet Pulsar
Authors: A. Albert, R. Alfaro, J. C. Arteaga-Velázquez, H. A. Ayala Solares, E. Belmont-Moreno, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño De León, E. De la Fuente, C. de León, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, C. Espinoza, K. L. Fan, N. Fraija, K. Fang, J. A. García-González, F. Garfias, A. Jardin-Blicq, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, Y. Pérez Araujo, Y. Son, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, R. W. Springer, K. Tollefson, I. Torres, R. Torres-Escobedo, X. Wang, K. Whitaker, E. Willox, H. Zhou
Figure caption: Left panel: spectral energy distribution (SED) of the emission around PSR J0359+5414, including the TeV halo (green and blue bands corresponding to the HAWC observation for a point-like and extended model, respectively, as explained in Section 3), the PWN (black band at 0.3–10 keV; Zyuzin et al. 2018), and the pulsar (in gray color; including the upper limit in radio at 1400 MHz from Grießmeier et al. (2021), the band in X-ray at 0.3–10 keV from Zyuzin et al. (2018), and the data points or limits at 100 MeV–1 TeV from Abdollahi et al. 2020). Right panel: SED of the emission around PSR B0355+54. The green and blue bands indicate the TeV excess emission obtained from fits to the HAWC data with models that center at B0355 with point-like and extended spatial profiles, respectively (see Appendix A). For comparison, the upper limits on VHE gamma-ray emission from the PWN by VERITAS with hard spectral cuts are shown in orange, with the upper and lower bars corresponding to region sizes of 0.°1 and 0.°235, respectively (Benbow et al. 2021). The black band at 0.5–8 keV indicates the PWN in X-rays (Klingler et al. 2016). The gray band at 0.5–8 keV (Klingler et al. 2016) and the circular data markers at 1400 and 1600 MHz (Lorimer et al. 1995) correspond to the emission from the pulsar. The HAWC bands correspond to statistical uncertainties only.
Paper: HAWC Detection of a TeV Halo Candidate Surrounding a Radio-quiet Pulsar
Authors: A. Albert, R. Alfaro, J. C. Arteaga-Velázquez, H. A. Ayala Solares, E. Belmont-Moreno, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño De León, E. De la Fuente, C. de León, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, C. Espinoza, K. L. Fan, N. Fraija, K. Fang, J. A. García-González, F. Garfias, A. Jardin-Blicq, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, Y. Pérez Araujo, Y. Son, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, R. W. Springer, K. Tollefson, I. Torres, R. Torres-Escobedo, X. Wang, K. Whitaker, E. Willox, H. Zhou
Figure caption: Comparison of the model maps, significance maps, and 1D residual histograms for point-like and extended spatial models. The source position is fixed to PSR J0359+5414 (black cross in the significance maps), and the spectrum is assumed to be a nonbroken power law. The best-fit parameter values are listed in Table 1.
Paper: HAWC Detection of a TeV Halo Candidate Surrounding a Radio-quiet Pulsar
Authors: A. Albert, R. Alfaro, J. C. Arteaga-Velázquez, H. A. Ayala Solares, E. Belmont-Moreno, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño De León, E. De la Fuente, C. de León, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, C. Espinoza, K. L. Fan, N. Fraija, K. Fang, J. A. García-González, F. Garfias, A. Jardin-Blicq, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, Y. Pérez Araujo, Y. Son, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, R. W. Springer, K. Tollefson, I. Torres, R. Torres-Escobedo, X. Wang, K. Whitaker, E. Willox, H. Zhou
Figure caption: HAWC significance map in Galactic coordinates using 2321 days of live data. The significance is computed with a point-like spatial template and a power-law spectrum with spectral index α = 2.7. For comparison, the positions of PSR J0359+5414 and PSR B0355+54 are marked.
Paper: Observational Evidence for Cosmological Coupling of Black Holes and its Implications for an Astrophysical Source of Dark Energy
Authors: Duncan Farrah, Kevin S. Croker, Michael Zevin, Gregory Tarlé, Valerio Faraoni, Sara Petty, Jose Afonso, Nicolas Fernandez, Kurtis A. Nishimura, Chris Pearson, Lingyu Wang, David L Clements, Andreas Efstathiou, Evanthia Hatziminaoglou, Mark Lacy, Conor McPartland, Lura K Pitchford, Nobuyuki Sakai, Joel Weiner
Figure caption: Cosmic star formation rate densities (SFRDs) capable of producing the necessary k = 3 BH density to give ΩΛ = 0.68 (green, solid). The details of the model are given in Appendix A. The upper bound of the viable region adopts a Kroupa (2002) initial mass function (IMF) at all redshifts with the least amount of remnant accretion required to produce ΩΛ with a decreasing power-law SFRD model (red, solid). The lower bound adopts the top-heavy IMF of Harikane et al. (2022a) at z > 7 (blue, solid). Two middle lines show the impact of a top-heavy IMF at z > 7, but no remnant accretion (green, solid); and higher accretion, but with a Kroupa IMF (orange, solid). Existing measurements of the SFRD via IR (Rowan-Robinson et al. 2018, red, squares), γ-ray bursts (Kistler et al. 2009, orange, stars), FIR (Algera et al. 2023, brown, xs), and rest-frame UV via the JWST (Harikane et al. 2022a; Donnan et al. 2022, purple, dots), (Bouwens et al. 2022, blue, dots) are over-plotted. The UV points can vary ∼−1 dex depending upon IMF assumptions and UV luminosity integration bounds. Consistency occurs with consumption of <3% of the baryon fraction Ω b  after cosmic dawn. The results assume stellar first light at z ⋆ = 25 (Harikane et al. 2022b, Figure 25) but are typical of the scenario for 15 < z ⋆ < 35. Also indicated are the redshifts probed by 21 cm experiments.