adsabs/AstroCLIMB huggingface dataset:
Paper: Selection of Dwarf Galaxies Hosting Active Galactic Nuclei: A Measure of Bias and Contamination Using Unsupervised Machine Learning Techniques
Authors: Sogol Sanjaripour, Archana Aravindan, Gabriela Canalizo, Shoubaneh Hemmati, Bahram Mobasher, Alison L. Coil, Barry C. Barish
Figure caption: WISE color W1 − W2 vs. stellar mass for the two SOM-identified clumps: right clump (blue circles) and left clump (red squares). The two populations show substantial overlap in W1 − W2 at fixed stellar mass, illustrating the difficulty of separating AGNs from star-forming dwarfs using WISE colors alone.
Paper: Investigating Little Red Dots with UV Excess: Are They the High-redshift Siblings of Blue Hot Dust-obscured Galaxies?
Authors: Lulu Bao, Chao-Wei Tsai, Jingwen Wu, Tao Wang, Guodong Li, Roberto J. Assef, Tanio Diaz-Santos, Peter R. M. Eisenhardt, Daniel Stern, Andrew W. Blain
Figure caption: The bolometric LFs of LRDs in higher and lower redshift bins reported by V. Kokorev et al. (2024) and J. E. Greene et al. (2024) are presented in diamonds and points, respectively. The pre-JWST bolometric LFs at z = 6 and z = 5, derived by X. Shen et al. (2020), are shown as dashed red and orange lines, respectively. The vertical green solid and dashed curves indicate the median bolometric luminosity of BHDs, with its 1σ scatter.
Paper: The ODYSSEUS Survey. Characterizing Magnetospheric Geometries and Hotspot Structures in T Tauri Stars
Authors: Caeley V. Pittman, Catherine C. Espaillat, Connor E. Robinson, Thanawuth Thanathibodee, Sophia Lopez, Nuria Calvet, Zhaohuan Zhu, Frederick M. Walter, John Wendeborn, Carlo F. Manara, Justyn Campbell-White, Rik Claes, Min Fang, Antonio Frasca, Jorge F. Gameiro, Manuele Gangi, Jesus Hernández, Ágnes Kóspál, Karina Maucó, James Muzerolle, Michał Siwak, Łukasz Tychoniec, Laura Venuti
Figure caption: Histograms of accretion flow model and stellar rotation results colored by region in order of approximate region age from youngest (yellow) to oldest (blue). Panels show (a) accretion rate, (b) accretion rate normalized by stellar mass according to ﹩\dot{M}\propto {M}_{\star }^{2}﹩, (c) maximum flow temperature, (d) inner magnetospheric truncation radius, (e) width of truncation region, and (f) magnetospheric inclination.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: High-resolution synthetic telluric spectrum from ATRAN (S. D. Lord 1992), colored by the dominant absorber at each wavelength. Blue indicates H2O and red indicates CO2. All other molecules contribute less than 1% absorption in this passband.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: Synthetic line profiles for the new coronal lines. The line profiles are modeled as Gaussians centered at the wavelengths in Table 2 with a width that includes thermal broadening and 25 km s−1 nonthermal broadening. The profiles are scaled by the telluric absorption spectrum shown in Figure 3. The radiance reduction and centroid shift due to telluric absorption are reported in each panel.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: SUMER spectra used for the wavelength calibration (prominence) and the measurement of the two Si XI coronal lines.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: Scatterplot of the difference between the SUMER wavelengths, fitted with a linear scale, and the reference (theor.) values, for a prominence region.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: Predicted radiances of the newly observed coronal lines.
Paper: New Near-infrared Coronal Lines Observed during the 2019 Total Solar Eclipse
Authors: Jenna Samra, Giulio Del Zanna, Celeste Elizalde Flores, Chad Madsen, Edward DeLuca
Figure caption: Gaussian fits to the new coronal lines.
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: Postshock energy vs. shock velocity inferred from peak properties of synchrotron-powered transients including Swift J1644 and AT 2022cmc (T. Eftekhari et al. 2018; B. Margalit & E. Quataert 2024). We find that AT 2022cmc has a similar outflow velocity compared to Swift J1644 and a higher total energy content. The maximum outflow velocity we derive is not high enough to match the lower limit found in L. Rhodes et al. (2023).
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: Top: the spherical outflow model fit (Section 4.2) to the data overlaid on the 1.28, 5, 15.5, and 101.75 GHz light curves. Bottom: the spherical outflow model fit to the data overlaid on the SEDs at ∼24, 160, 370, and 910 days postdiscovery. The model tends to underpredict the earliest high-frequency and late-time 1.28 GHz data; however, this remains our best-fit model.
Paper: Bondi-like Accretion Flow Dynamics: The Role of Gravitational Potential
Authors: Razieh Ranjbar, Héctor R. Olivares-Sánchez, Shahram Abbassi
Figure caption: Mhalo = MBH, a0 = 50, Variations of accretion rate as a function of temperature at the outer boundary in different gravitational potentials and rotation. The filled black diamonds represent the accretion model with zero angular momentum in the Paczyński–Wiita potential of the BH, while the yellow dots include the effects of the generalized Newtonian potential (E. Tejeda & S. Rosswog 2013). Filled pink stars are the Bondi model with galaxy potential. Filled blue squares include DM potential. Filled violet circles are both of them. Finally, filled red triangles show the accretion model with low angular momentum.
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: The radio and submillimeter light curve for AT 2022cmc between 100 and ∼1000 days postdiscovery. At the highest frequencies, 86.26 and 101.75, the light curve follows a power-law decay. At lower frequencies (15.5 GHz and below), the light curves are best described by a broken power law. We quantify the rise and decay rates at each frequency in Section 3.
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: SEDs constructed using data in Figure 1 at 120, 160, 260, 270, 600, and 720 days postburst. There is a clear shift of the spectral peak over the duration of our campaign from above 15.5 GHz (<300 days) to around 3 GHz (∼900 days).
Paper: Thermal Electrons in the Radio Afterglow of Relativistic Tidal Disruption Event ZTF22aaajecp/AT 2022cmc
Authors: Lauren Rhodes, Ben Margalit, Joe S. Bright, Hannah Dykaar, Rob Fender, David A. Green, Daryl Haggard, Assaf Horesh, Alexander J. van der Horst, Andrew K. Hughes, Kunal Mooley, Itai Sfaradi, David Titterington, David Williams-Baldwin
Figure caption: Top: the jetted outflow model (Section 4.3) considering both nonthermal and thermal electrons with the data overlaid on the 1.28, 5, 15.5, and 101.75 GHz light curves. Bottom: the jetted outflow model fit to the data overlaid on the SEDs. Given the scatter in the model, we only model the SEDs at ∼24, 160, 370, and 910 days postdiscovery to prevent overcluttering the figure. The jetted model cannot explain the steep spectral index, the high-frequency turnover in the first ∼10 days postdiscovery, or the low-frequency emission.
Paper: Bondi-like Accretion Flow Dynamics: The Role of Gravitational Potential
Authors: Razieh Ranjbar, Héctor R. Olivares-Sánchez, Shahram Abbassi
Figure caption: The dependence of accretion rates on the temperature at the outer boundary. We set the gas density at the outer boundary to be 10−24 gr cm−3. Red lines mean the accretion rates ﹩\dot{M}/{\dot{M}}_{{\rm{Edd}}}﹩ predicted by our models, while blue lines mean ﹩\dot{M}/{\dot{M}}_{{\rm{Bondi}}}﹩. Black dotted lines mean the changing trend of the accretion rates predicted by the Bondi model.
Paper: Bondi-like Accretion Flow Dynamics: The Role of Gravitational Potential
Authors: Razieh Ranjbar, Héctor R. Olivares-Sánchez, Shahram Abbassi
Figure caption: Mass accretion rate in units of Eddington accretion rate as a function of angular momentum at the outer boundary ﹩{ \mathcal L }\gt 1﹩. The orange dots are for a0 = 100,  Mhalo = MBH, and the blue line is the case without DM potential.
Paper: Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: The top row shows the spectra where we have assumed that the nonthermal electron distribution responsible for the gyrosynchrotron emission follows a power-law distribution. The bottom row shows the thermal gyroresonance emission spectrum from a thermal distribution of electrons. The red points in the left and right columns show the observed spectra at 00:00:02 and 00:16:05 UT (refer to Figure 5).
Paper: Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Spectra for different times are shown. The region from which the spectrum has been extracted is shown with an ellipse over the image at the corresponding time in Figure 4. Circles and triangles show the detections and upper limits, respectively.
Paper: Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: The top four rows show OVRO-LWA radio images at a few example frequencies and times during the WL CME. The time corresponding to each column is indicated at the top of each column. The contour levels are at 0.02, 0.04, 0.08, 0.16, 0.32, 0.64, and 1 MK. In the bottom row, we have shown the nearest white-light image from the LASCO C2. The time corresponding to the white-light image is written in each panel. The magenta ellipse in each panel shows the region from which the spectrum, shown in Figure 5, has been extracted.
Paper: Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: OVRO-LWA 39 and 80 MHz contours overlaid on LASCO C2 images at multiple timestamps beginning at a time when the CME is not yet in the LASCO C2 field of view, until the time of sunset at the observatory. The 39 and 80 MHz contours are drawn at 0.07 and 0.025 MK, respectively. The title of each panel shows the time of the radio image. The time written inside each panel shows the time of the background white-light image, which is shown in inverted grayscale (i.e., the dark color is brighter). Due to the limited time cadence of LASCO C2, the nearest available white-light image is chosen as the background.
Paper: HAWC Performance Enhanced by Machine Learning in Gamma-hadron Separation
Authors: R. Alfaro, C. Alvarez, A. Andrés, E. Anita-Rangel, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, E. De la Fuente, D. Depaoli, P. Desiati, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, N. Ghosh, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, D. Huang, P. Hüntemeyer, A. Iriarte, S. Kaufmann, D. Kieda, K. Leavitt, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, P. E. Mirón-Enriquez, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Najafi, A. Nayerhoda, L. Nellen, N. Omodei, M. Osorio, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, H. Salazar, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, H. Zhou, C. de León
Figure caption: Spectral energy distribution of the Crab Nebula. The plot compares different analysis methods and data sets, including a Pass 5 fHit bins with ML (black line) and a Pass 5 fHit bins with SC (red line). Shaded bands indicate the corresponding statistical uncertainties. LHAASO-WCDA and LHAASO-KM2A data are represented by orange triangles and brown squares, respectively (LHAASO Collaboration et al. 2021).
Paper: Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Left panel: Location of Solar Orbiter, Earth, and Sun. Middle and right panel: SolO/FSI 304 Å images at two different times showing the early times of the solar eruption. The time indicated on the title of the panels shows the observation time, after correcting for the light travel time between SolO and Earth.
Paper: Possible First Detection of Gyroresonance Emission from a Coronal Mass Ejection in the Middle Corona
Authors: Surajit Mondal, Bin Chen, Xingyao Chen, Sijie Yu, Dale Gary, Peijin Zhang, Marin M. Anderson, Judd D. Bowman, Ruby Byrne, Morgan Catha, Sherry Chhabra, Larry D'Addario, Ivey Davis, Jayce Dowell, Katherine Elder, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Jack Hickish, Rick Hobbs, David Hodge, Mark Hodges, Yuping Huang, Andrea Isella, Daniel C. Jacobs, Ghislain Kemby, John T. Klinefelter, Matthew Kolopanis, Nikita Kosogorov, James Lamb, Casey Law, Nivedita Mahesh, Brian O'Donnell, Kathryn Plant, Corey Posner, Travis Powell, Vinand Prayag, Andres Rizo, Andrew Romero-Wolf, Jun Shi, Greg Taylor, Jordan Trim, Mike Virgin, Akshatha Vydula, Sandy Weinreb, Scott White, David Woody, Thomas Zentmeyer
Figure caption: Shows the dynamic spectrum from OVRO-LWA in uncalibrated units. The red vertical lines show the times within the interval shown for which we find spectra consistent with gyroresonance origin. There is also a data gap between 22:56 and 23:24 UT, and it has been darkened.
Paper: On the Formation of Star-forming Galaxies Having Anomalously Low-metallicity Regions: The Role of Galaxy Interaction and Circumgalactic Medium/Intergalactic Medium Accretion
Authors: Yibo Cao, Zhizheng Pan
Figure caption: Similar to Figure 10, but with the O3N2 calibrator.
Paper: On the Formation of Star-forming Galaxies Having Anomalously Low-metallicity Regions: The Role of Galaxy Interaction and Circumgalactic Medium/Intergalactic Medium Accretion
Authors: Yibo Cao, Zhizheng Pan
Figure caption: Similar to Figure 9, but with the O3N2 calibrator.
Paper: On the Formation of Star-forming Galaxies Having Anomalously Low-metallicity Regions: The Role of Galaxy Interaction and Circumgalactic Medium/Intergalactic Medium Accretion
Authors: Yibo Cao, Zhizheng Pan
Figure caption: Similar to Figure 7, but with the O3N2 calibrator.
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: The ratio between the radio and IR fluxes, normalized by the ratios of their frequencies, plotted against αIR-X defined in Equation (1). BL Lac objects in ROMA-BZCAT are displayed as yellow triangles, while FSRQs are displayed as blue triangles. The 21 TeV-detected HBLs within the eROSITA footprint are shown as unfilled red triangles, while the ones designated as extreme HBLs (eHBLs) in TeVCat are shown as filled red triangles. The 135 candidate sources identified in our study are shown as open black circles. Sources that have passed all previous candidacy criteria but have αR-IR ≤ 0.43 are designated as green circles outlined in black.
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: The WISE 3.4–4.6–12 μm color–color plot for the 56 TeV HBLs selected (red crosses). The dashed line corresponds to the regression line described in Section 2. The black dashed rectangle corresponds to the maximum allowed separation (0.21) of the known TeV HBLs from this line. The turquoise points correspond to all WISEA sources found within the eROSITA footprint.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: Description of the algorithm followed to identify TeV-emitting HBL candidates. The input surveys WISEA and eRASS1 are shown at the top in light blue. The resulting outcome of 135 objects is shown at the bottom, also in light blue. The number of objects that make it through each stage of filtering is shown in red boxes. Green boxes indicate parameters that are calculated based on catalog inputs.
Paper: New TeV-emitting BL Lac Candidates from the eROSITA X-Ray Survey
Authors: Cassidy Metzger, Andrea Gokus, Manel Errando
Figure caption: The distribution of αIR-X for all sources found in eRASS1 and WISEA (blue) and the 21 TBL sources found in the eRASS1 footprint (red). The dashed black line represents our selection criterion of αIR-X ≤ 1.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Fluorescence spectrum of H2 at a resolution of R = 1000 produced by our Meudon PDR model. Using this spectrum, we can then identify the strongest features and compare to observations. The upper wavelength range assumes a redshift z = 10.6, which is the highest redshift source in our sample.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Continuum-subtracted stacked spectrum (top row) and the signal-to-noise ratio (bottom row) of all JWST JADES galaxies with redshifts z ≥ 7, investigating the tentative detections of C IV, H2 Fluorescence, He II, O III], and C III]. These potential detections hint at the presence of multiphase outflows at cosmic dawn through slightly shifted emission peaks and P Cygni–like profiles.
Paper: Detecting Molecular Hydrogen (H2) Emission at Cosmic Dawn
Authors: Madisen Johnson, Blakesley Burkhart, Francesco D'Eugenio, Sandro Tacchella, Roberto Maiolino, Shmuel Bialy, Jacques Le Bourlot, Evelyne Roueff, Franck Le Petit, Emeric Bron, Hervé Abgrall, Erica Nelson, Shyam Menon, Matthew E. Orr
Figure caption: Comparison of the potential stacked H2 fluorescent emission feature with our high-redshift Meudon PDR model (blue line) and predicted features (red vertical lines), which have now been shifted by 0.18 nm or ∼340 km s−1 to better match the observed spectrum. This displays the unique profile of the potential detection, which could indicate the presence of molecular outflows.