adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution, Structure, and Topology of Self-generated Turbulent Reconnection Layers
Authors: Raheem Beg, Alexander J. B. Russell, Gunnar Hornig
Figure caption: Comparison of color maps ﹩{C}_{{z}_{0}}^{n}﹩ at t = 3.0. The top and bottom panels show n = 1 and n = 10 at z 0 = −0.5, respectively. Although we can identify flux rope structures within the stochastic field, the field line mapping is too topologically complicated to allow for the detection of distinct flux ropes using color maps, presumably because they are too small or not structured around a periodic point.
Paper: Preemergence Signatures of Horizontal Divergent Flows in Solar Active Regions
Authors: T. Rees-Crockford, C. J. Nelson, M. Mathioudakis
Figure caption: Evolution of the relevant magnetic field (red lines) and Doppler velocity (dashed blue lines) windows for the three ARs compared to Toriumi et al. (2014; as discussed in Section 3.1). The counts have been normalized against the standard deviations calculated from the initial 3 hr background time. The flux emergence above 1σ is clear in each event (denoted by the vertical solid black lines), with the presence of the HDF also being apparent in the Doppler data for ARs 11066 and 11072 (denoted by the vertical dotted–dashed black lines). No HDF is detected for AR 11076.
Paper: Preemergence Signatures of Horizontal Divergent Flows in Solar Active Regions
Authors: T. Rees-Crockford, C. J. Nelson, M. Mathioudakis
Figure caption: (Left panel) Flowchart of the determination of the time of magnetic emergence, T FE. (Right panel) Flowchart of the determination of the Doppler time of preemergence, T DE, for both methods used here. Note that for all cases the profiles used here are those of the residual profiles discussed in Figure 2.
Paper: Preemergence Signatures of Horizontal Divergent Flows in Solar Active Regions
Authors: T. Rees-Crockford, C. J. Nelson, M. Mathioudakis
Figure caption: Flowchart of the data extraction method for both the magnetic field strength and Doppler velocity data sets.
Paper: Preemergence Signatures of Horizontal Divergent Flows in Solar Active Regions
Authors: T. Rees-Crockford, C. J. Nelson, M. Mathioudakis
Figure caption: [16:] Top row: The mean residual counts across the velocity profile for AR 11066 at the shown time showing a “center” increase (left) and for AR 11088 showing a “wings” increase (right). In both panels, the vertical lines denote the wing/center limit, ±0.3 km s−1. Bottom: Longitude vs. AR. The color and shape are coded by trend type, where red circles show center trends, and blue squares [16:] and diamonds show wing trends. The gray lines are to help guide the reader’s eye.
Paper: Preemergence Signatures of Horizontal Divergent Flows in Solar Active Regions
Authors: T. Rees-Crockford, C. J. Nelson, M. Mathioudakis
Figure caption: As Figure 4, but for the 12 minute cadence data. The general behavior of the ARs is consistent with the full-cadence data with only minor changes to the results returned.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Top: the Fermi-LAT light curve for V392 Per. Photon flux is calculated over the energy range 0.1–300 GeV. The upper limits plotted are 95% CLs. Bottom: the optical V-band light curve of V392 Per over the same window of time as measured by the American Association of Variable Star Observers (AAVSO).
Paper: The Correlation between WISE 12 μm Emission and Molecular Gas Tracers on Subkiloparsec Scales in Nearby Star-forming Galaxies
Authors: Yang Gao, Qing-Hua Tan, Yu Gao, Min Fang, Ryan Chown, Qian Jiao, Chun-Sheng Luo
Figure caption: Spectra of 12CO (red thin lines) and 13CO (blue thick lines) in the regions of NGC 4736 (top), NGC 5457 (bottom left), and M51 (bottom right) observed with PMO. The temperature of 13CO is timed by 5 for direct comparison. We also derive the simulated PMO 12CO spectra (gray thick lines) from the literature one (Kuno et al. 2007) based on the parameters of PMO and the NRO45M telescope. All spectra are on the T mb scale and smoothed to a velocity channel width of ∼10 km s−1 for display. The S/N of 12CO and 13CO emission and offset from the center of galaxy are indicated in each box.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: The Fermi-LAT SED for V392 Per. Upper limits in the lowest- and highest-energy bins signify 95% confidence limits (CLs).
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: HAWC upper limits on the SED corresponding to S 95 during the “On” period, when varying the PL index within Γ = 2–4 in steps of 0.2 (limits for 2.0, 3.0, and 4.0 are noted specifically). The upper horizontal line, in orange, denotes the Fermi-LAT best-fit SED extrapolated to high energy.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: The γ-ray SED of V392 Per, based on the Fermi-LAT detections and HAWC 95% upper limits. Γ = 2.0 refers to a local PL assumed within a HAWC energy bin in the limit calculation.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Expected and observed limits vs. energy for V392 Per. The observed limit is in black and the median expected limit is a dashed line in red. The central green band covers 68% of the expected limits (1σ) while the outer yellow bands cover 95% (2σ).
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: HAWC significance map of V392 Per during the week of Fermi-LAT detection (i.e., the “On” period). The position of the nova is indicated by a cross. HAWC pointing at this decl. is accurate to better than 0.°1.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Daily significance of V392 Per from 2018 April 22 to May 31 in HAWC data, assuming a Γ = 2.0 PL spectrum. The vertical lines bound the “On” period of observation, coincident with the Fermi-LAT GeV detection.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Optical depth in the vicinity of the γ-ray generating shock τ  γ γ  as a function of time, with different γ-ray energies shown as lines of different colors as marked. The opacity is due to γ γ pair creation on the target background radiation of the nova optical light. The results shown in the top panel assume the spectrum of the optical radiation is that of a blackbody at T eff ≈ 8000 K, while the bottom panel assumes a free–free emission spectrum of gas at the same temperature (accounting for self-absorption at low frequencies). These two choices roughly bracket the expected level of attenuation for the more realistic but complex optical spectral shape in novae. Epochs when τ  γ γ  > 1 may have their γ-ray emission strongly attenuated close to the source, where τ  γ γ  = 1 is given by the dotted line.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Top: the evolution of V392 Per’s Hα line profile near the optical peak. The numbers in brackets represent days relative to the peak. The radial heliocentric velocities are derived relative to the line center, which is marked by a red dashed line. The blue, black, and green dashed lines represent v 1 = 2700 km s−1, v 2 = 3800 km s−1, and v 3 = 5500 km s−1 relative to the line center, respectively. Bottom: a zoomed-in view of the absorption components for the day +1 spectrum.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Top: for each of the 15 γ-ray detected novae, the duration over which Fermi-LAT achieved >2σ detections is plotted against the time for the optical light curve to decline by 2 mag from maximum (t 2). Bottom: γ-Ray duration plotted against the total energy emitted during this time integrated over the LAT bandpass. In both panels, V392 Per is plotted as a red point.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: Top: optical light curve of V392 Per, measured in the B, V, R, and I bands by the AAVSO. Bottom: V392 Per’s bolometric luminosity as a function of time, estimated from integrating the optical SED.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: The γ-ray SED of nova V339 Del, with Fermi-LAT detections in yellow and MAGIC limits in black. Superimposed is the SED of V392 Per (red and green), with HAWC limits for V392 Per using the same Γ = 2.3 PL index as MAGIC.