adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Flux as a function of FWHM for all detected objects in a single tile of the F200W image (∼0.019 deg2), measured using measure_FWHM function in galight. CW-LRD-z10 exhibits an FWHM consistent with the sequence of point sources, strongly suggesting that it is a very compact object similar to previously found LRDs.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: HSC (grizy), HST (F814W), and JWST ﹩2\mathop{.}\limits^{^{\prime\prime} }5\times 2\mathop{.}\limits^{^{\prime\prime} }5﹩ cutout images centered on each object excluded in visual inspection. For comparison, we also plot CW-LRD-z10 (ID:426069). Each image is scaled by a noise map.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Completeness as a function of redshift and UV absolute magnitude, estimated from a Monte Carlo simulation of COSMOS-Web mock observations.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Top: Kippenhahn diagram of the primary star of the M1,init = 1.1 M⊙, qinit = 0.75, pinit = 0.67 day model with ET and saturated MB during the first few TROs. Middle: strength of the MB and GR AML. Bottom: radius evolution. The drop in MB strength, indicated by the gray vertical bar, is commensurate with the ﹩\exp (-1)﹩ factor introduced by shallow convective envelopes (see Section 3.2).
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Lifetimes of the contact phases of the models with qinit = 0.75. We confirm our estimates from Section 2 that models using the classical MB law have a lifetime of only 107 yr, while saturated MB allows for lifetimes longer than 108 yr. The fact that the ET and no-ET models have largely the same lifetimes is coincidental. For the models undergoing TROs (see Figure 4), the lifetimes reported here are lower limits.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Mass-transfer rate, radius, and mass-ratio evolution of the M1,init = 0.9 M⊙, pinit = 0.67 day, qinit = 0.75 models with saturated MB, with ET (red curves), and without ET (blue curves). Without ET, the system merges at a mass ratio of unity after MT is engaged, while the model with ET evolves away from mass-ratio unity and develops TROs (see inset).
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Mass-transfer rate, radius, and mass-ratio evolution of the M1,init = 0.9 M⊙, pinit = 0.67 day, qinit = 0.75 models without ET under the different MB laws. We note that the saturated MB model has its total lifetime as well as its time in binary interaction increased by about an order of magnitude.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Termination of the q = 0.75 models of our grids as a function of initial primary mass M1,init and initial period p. Termination conditions are listed in Section 3.4. We note that only the combination of ET and saturated MB allows models over a wide parameter range to experience TROs.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Probability density of our model grids. The top panels show the marginalized mass-ratio distributions, while the lower panels show the two-dimensional (p, qobs) distributions. We note that only the models with ET and saturated MB are able to produce systems with mass ratios significantly different from unity.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Mass-ratio extrapolation of the example model of Section 4.1. We find that if the system remains stable, it would reach the critical mass ratio ﹩{q}_{{\rm{\min }}}﹩ after around 0.7 Gyr in contact.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Volume-equivalent radius ratio of the L2 and Roche-lobe (RL) equipotentials as a function of the mass ratio. This function is discontinuous at q = 1 because the location of L2 moves from the far side of M2 to the near side of M1.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Top: Ledoux (∇L) and radiative temperature gradients (∇rad) as a function of the mass coordinate for the lower-mass component in the contact (red) and semidetached (blue) phases of the TROs. Bottom: luminosity profile of the envelope. During the contact phase, the radiative gradient is suppressed by a decrease in internal luminosity.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: M–R curves for the selected super-puffs and young planets. We show planetary radii at different pressure levels (color-coded). The width of each shaded region reflects the variation in radius due to uncertainties in system age. For Kepler-51 planets, only the lower-bound radii at pressure levels other than 1 nbar are shown (dotted). We also display the 1 nbar radius at the best-fit system age (dashed). See the main text for further discussion.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Comparison of radial profiles for temperature (top left), Mach number (top right), density (bottom left), and ionization fraction (bottom right) between a super-puff (black, Kepler-51b) and a hot Jupiter (red, HD 209458b). The photoionization base is marked with circles. Structures are shown from the 1 μbar level (triangles) to the sonic point (crosses). See the main text for further discussion.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Modeled evolutionary tracks of planetary radii and H/He mass fractions (defined as the ratio of H/He mass and total planetary mass) for the sample super-puffs and young planets in Table 1. Note that the x-axis scale varies between panels, reflecting differences in cooling and mass-loss timescales. Radii at various pressure levels are shown, along with observational data points for comparison. For clear atmospheres, the transit pressure typically lies at the mbar level, while hazy atmospheres push this pressure down to the nbar range. Planetary age is defined as the time elapsed since the dispersal of the inner disk. Circles in the H/He mass fraction panels indicate the epoch corresponding to the observational data.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: In the top panel, we display the thermal-energy-mediated (red) and energy-limited (blue) mass-loss rates, based on Equations (23) and (11), respectively. For comparison, the mass-loss rate from our numerical model is shown with a black dashed line. The kinks in the mass-loss rate reflect the evolution of the EUV flux, which remains saturated during the early stages. In the bottom panel, we plot the evolution of the escape parameter at the sonic point (Rs, black) and at the wind base (Rbase, gray).
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: 1 μbar radii calculated from the isothermal Parker wind (gray) and our nonisothermal, hydrostatic atmosphere (black), which serves as the fiducial model for determining optical radii. The transition between these two regimes (red) ensures a proper estimate of the lower-boundary radius for the photoevaporation model.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Comparison of planetary evolution for Kepler-51b during the photoevaporation phase between our new framework (black) and the previous framework (gray), which assumes a constant scale height for the radiative atmosphere and energy-limited escape. The top panel presents the 20 mbar (solid) and 1 nbar (dashed) radii. For consistency in comparison, both models start with the same initial conditions, self-consistently calculated from a boil-off phase. In contrast, the previous framework treats initial conditions as free parameters, whose effects are not shown in the figure. See the text for further discussion.
Paper: Contact-binary Evolution with Energy Transfer and Saturated Magnetic Braking
Authors: Matthias Fabry, Andrej Prša
Figure caption: Radius of the primary (top) and mass-ratio evolution (bottom) under different prescriptions for the width of the ET region. The narrow model promptly starts TROs when contact is engaged, while wider ET models have a short quasi-stable phase.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Comparison of energy budgets for high-gravity (top) and low-gravity (bottom) planets, corresponding to the same planets shown in Figure 2. Refer to the main text for a detailed discussion.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: The top panel shows the bulk density as a function of planetary mass (x-axis), with bolometric flux color-coded. For comparison, we overlay two sets of observations of the Kepler-51 planets, one from inner resonance (gray circles) and the other from outer resonance (black circles). The bottom panel presents the relative physical sizes of the envelope (solid) and radiative atmosphere (dashed), both normalized by the total planetary radius. This analysis assumes a hazy atmosphere with a transit pressure at 1 nbar, which is found to be likely for Kepler-51d in Figure 7.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: M–R curves (left panel) and gas mass fraction as a function of planetary mass (right panel), with varied metallicity (color-coded) ranging from 1 to 100 times the solar value. Solid curves include both boil-off and photoevaporation, similar to Figure 9, while dotted curves assume constant compositions for comparison purpose. System ages are set to the observational lower bounds: 200 Myr for Kepler-51d and 5.68 Gyr for Kepler-87c. The results indicate that super-puffs likely have low atmospheric metallicity. See the main text for further discussion.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: M–R curves for Kepler-223 planets. The 1 nbar (pink) and 20 mbar (purple) radii correspond to hazy and clear atmospheres, respectively. The envelope-free phase is indicated by the gray shaded region. Planets are expected to evolve rapidly toward a thin-atmosphere rocky state, represented by the red dashed curve, following the green dashed trajectory. Observational uncertainties in mass and radius are shown as error bars on the black data points, while uncertainties in age contribute to the dispersion of the M–R curves. The best-fit age is marked by dashed lines. Our model results suggest that the currently reported mass measurements for the Kepler-223 planets are inconsistent with their expected evolutionary paths and likely underestimate the true masses.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: M–R curves for planets orbiting Sun-like stars, shown as a function of incident flux (different columns), age (top row), and pressure level (bottom row). The pressure level is fixed at 10 nbar in the top panels, and the age is fixed at 500 Myr in the bottom panels. Notably, we find that boil-off in planets receiving 1000 F⊕ is highly sensitive to mass, resulting in distinct kinks in the curves. This behavior warrants further physical investigation. The transformation boundary, marking the transition to an envelope-free state, results in the truncation on the left. Accurately determining this boundary requires a large set of models with varying masses and ages; thus we have only calculated this boundary with a precision of 0.5 M⊕.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Tidal heating normalized by the total interior cooling as a function of planet mass for Kepler-51b. Three types of tides are considered here at the observed age: obliquity tide (gray), synchronization tide in the envelope (black), and synchronization tide in the rock/iron core (red).
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Comparison of heating profiles from Model A (solid) and Model B (dashed), both with the same mean molecular weight, for Kepler-51d at 100× solar metallicity. Model A achieves the target molecular weight by adjusting the H/He mass ratio, while Model B retains the unadjusted solar H/He mass ratio and instead varies the hydrogen atomic mass.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Temperature at the sonic point as a function of the EUV flux. The analytical fit is shown in black, and the data points are color-coded.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: Atmospheric escape parameter at the wind base as a function of flux and gravity (left) and envelope radius reduction following boil-off (right), for the same sample of planets shown in Figure B1 and B2.
Paper: Understanding the Origins of Super-puff Planets: A New Mass-loss Regime Coupled to Planetary Evolution
Authors: Yao Tang, Jonathan J. Fortney, Ruth Murray-Clay, Madelyn Broome
Figure caption: The ratio of the sonic radius to the photoionization base radius at the transition between the two mass-loss regimes, as a function of the logarithm of bolometric flux. The analytical fit is shown in black and the data points are color-coded.
Paper: Fermi-LAT Captures a Late-2024 Gamma-Ray Outburst near Two Newly Identified Gamma-Ray-emitting Galactic Supernova Remnants, without Evidence of Physical Association
Authors: Miltiadis Michailidis, Marianne Lemoine-Goumard, Niccolo Di Lalla, Nicola Omodei, C. C. Cheung, Guillem Marti-Devesa, Denis Bernard
Figure caption: The 10° × 10° Fermi-LAT PS maps, expressed in sigmas (σ) and for energies >1 GeV, are centered at G093.7–00.2. PS maps are deviation probability maps that offer an accurate data and model comparison by being sensitive to both positive and negative deviations (P. Bruel 2021). Coordinates are given in degrees. The model excludes only the spatially coincident 4FGL J2123.9+5158 source with the 3C 434.1 SNR. Circles indicate the positions of the two SNRs and the outburst event (located ﹩\sim 0\mathop{.}\limits^{^\circ }26﹩ above the Galactic plane). Yellow crosses indicate 4FGL-DR4 sources within the ROI. The upper left panel presents the Fermi map for the entire 16.5 yr time range. The upper right panel displays the Fermi map with the first 14 yr of data from August 8, 2008, to August 8, 2022 (MET: 239557417 to 681320621). The lower left panel shows the Fermi map with the last 2.5 yr of data from August 8 2022, to February 13, 2025 (MET: 681320621 to 761167438). The lower right panel illustrates the Fermi map with 5 days of data from August 5, 2024, to August 10, 2024 (MET: 744552005 to 744984005) centered on the event peak.
Paper: On the Fate of Little Red Dots
Authors: Andrés Escala, Lucas Zimmermann, Sebastián Valdebenito, Marcelo C. Vergara, Dominik R. G. Schleicher, Matías Liempi
Figure caption: Total masses M and sizes R in color points for the following systems: resolved MBHs (black), unresolved MBHs (white), NSCs (orange), and LRDs (red). The solid black curve follows the condition tcoll(M, R) = tH0 for a system of a given mass M and radius R (at the current age of the Universe tH0 = 1.4 × 1010 yr), and the dashed one follows the condition trelax(M, R) = tH0. The color diagram denotes the BH efficiency expected from ﹩{\epsilon }_{\mathrm{BH}}={\left(1+\exp \left[-4.63\left(\mathrm{log}\left(M/{M}_{\mathrm{crit}}\right)-4\right)\right]\right)}^{-0.1}﹩ (M. C. Vergara et al. 2023, 2024, 2025a), with Mcrit coming from the condition tcoll (Mcrit) = tH0. Those efficiencies match the expectations for the MBH formation scenario outlined in A. Escala (2021), where MBHs are formed from (partially/totally) failed stellar systems, by approaching 1 for resolved MBHs (black points) and being NSCs mainly in the range between 0.05 and 0.15 (coexistence of an MBH and an NSC; A. Escala 2021). The region called “Forbidden Stellar Zone” fulfills the instability defined by tcoll < tH0 ( < trelax), where no stellar system is expected to survive, with most LRDs being at the boundary of such instability (within 1 order of magnitude if we consider their upper limits in total effective radius).
Paper: On the Fate of Little Red Dots
Authors: Andrés Escala, Lucas Zimmermann, Sebastián Valdebenito, Marcelo C. Vergara, Dominik R. G. Schleicher, Matías Liempi
Figure caption: (a) Total masses M and radius R in red points for LRDs, with the solid black curve following the condition tcoll(M, R) = tH0 for the age of the Universe at z ∼ 8 (tH0 = 0.6 × 109 yr) and the dashed one following the condition trelax(M, R) = tH0. The color diagram denotes the predicted BH mass MBH expected from ﹩M\times {\left(1+\exp \left[-4.63\left(\mathrm{log}\left(M/{M}_{\mathrm{crit}}\right)-4\right)\right]\right)}^{-0.1}﹩ (M. C. Vergara et al. 2023, 2024, 2025a), predicting MBH at an approximate range between 5 × 106and 1010 M⊙. (b) The positions of LRDs for the measured upper limit radius are shown in red, LRDs positions assuming that their real effective radii corresponds to the 10% of the upper limits in green, and assuming that corresponds to the 1% of the upper limits in radius in cyan. The solid and dashed black curves denote the same condition as in (a) but at the cosmic age of appearance (tH0 = 0.6 × 109 yr) and disappearance (tH0 = 1.5 × 109 yr) of LRDs. In the case of the green points, a fraction enters the “Forbidden Stellar Zone” (tcoll < tH0 < trelax), while the cyan points that it is more extreme, with most LRDs in such a situation. (c) Same as (b) but now assuming that it is the core radius of the LRDs that equals 10% (green) or 1% (cyan) of their measured effective radii, with most of the cores entering the “Forbidden Stellar Zone” in the case where the LRD core radius equals 1% of their measured radii.
Paper: Fermi-LAT Captures a Late-2024 Gamma-Ray Outburst near Two Newly Identified Gamma-Ray-emitting Galactic Supernova Remnants, without Evidence of Physical Association
Authors: Miltiadis Michailidis, Marianne Lemoine-Goumard, Niccolo Di Lalla, Nicola Omodei, C. C. Cheung, Guillem Marti-Devesa, Denis Bernard
Figure caption: The Fermi-LAT PS maps, expressed in sigmas (σ) and for energies >1 GeV, are centered on the SNRs 3C 434.1 (left panel) and G093.7–00.2 (right panel). Coordinates are given in degrees. The white contours delineate the CGPS radio extensions of the SNRs in their respective panels. The best-fit location and extension of the gamma-ray sources are displayed in green. There is no measured extension for G093.7–00.2. The prominent feature in the upper right corner of the right panel map corresponds to the gamma-ray counterpart of 3C 434.1.