adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption: XMM-Newton EPIC and NuSTAR spectra fit with four phenomenological models. From top left to top right: (1) an absorbed power-law model fit; (2) an absorbed power law fitted with a Gaussian at 6.4 keV component; (3) an absorbed APEC model fit; and (4) an absorbed APEC model with a Gaussian at 6.4 keV component. The NuSTAR observation used here is 30901021002 and is presented in the 3–50 keV band, with FPMA (1146 counts) in black and FPMB (1097 counts) in red. The XMM-Newton observation 0553950201 is presented in the 1.5–10 keV band with MOS1 (1438 counts) in magenta and MOS2 (1342 counts) in yellow. The more recent XMM-Newton observation 0870990201 is presented in the 0.5–10 keV band with MOS1 (667 counts) in green, MOS2 (671 counts) in navy blue, and PN (1688 counts) in light blue.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption:                    ﹩{Z}_{3}^{2}﹩ periodograms (top) and pulse profiles folded by their peak period (bottom) and reference time at T 0 = 55197 MJD. From left to right: 0553950201 MOS1, 0870990201, MOS1 and 0870990201 PN. In each periodogram, 3σ and 5σ significance levels are marked by solid and faded lines, respectively. In the pulse profile plots, the red horizontal lines indicate the mean counts per phase bin, and 1σ error bars are included at ϕ = 0 − 1.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption:  MCVSPEC model spectrum with M = 1M ⊙ and ﹩\dot{m}=1﹩ g cm−2 s−1 and R  m /R = 20.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption:                    ﹩{Z}_{3}^{2}﹩ broadband (0.5 mHz–2 Hz) periodograms. From left to right: 0553950201 MOS, 0870990201 MOS, and 0870990201 PN. In each periodogram, 3σ and 5σ significance levels are marked by solid and faded lines, respectively. The most significant peak is in the region of P ∼ 614 seconds. The first observation significantly detected a peak at 1227 s, which was less significantly detected in later observations.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption: XMM-Newton and NuSTAR spectra and residuals of J1745−3213 fit with a tbabs ∗ pcfabs ∗ (APEC+gauss) model, which yielded a ﹩{\chi }_{\nu }^{2}=1.00﹩ for 376 degrees of freedom and strongly supports the IP scenario. The Gaussian line fitted at 6.4 keV and modeling the Fe K emission line yielded an equivalent width of ﹩{146}_{-49}^{+68}﹩ eV, which is typical of IPs.
Paper: Constraining the White-dwarf Mass and Magnetic Field Strength of a New Intermediate Polar through X-Ray Observations
Authors: Benjamin Vermette, Ciro Salcedo, Kaya Mori, Julian Gerber, Kyung Duk Yoon, Gabriel Bridges, Charles J. Hailey, Frank Haberl, Jaesub Hong, Jonathan Grindlay, Gabriele Ponti, Gavin Ramsay
Figure caption: XMM-Newton and NuSTAR spectra fit by tbabs ∗ pcfabs ∗ (reflect ∗ MCVSPEC+gauss) and residuals for R M/R = 20. Top left: ﹩\dot{m}=0.6﹩ g cm−2 s−1; top right: ﹩\dot{m}=3.0﹩ g cm−2 s−1; bottom left: ﹩\dot{m}=10﹩ g cm−2 s−1; bottom right: ﹩\dot{m}=44﹩ g cm−2 s−1.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Visualization of TuRBO over the 2D space. The goal is to find the optimal (ΔΠ1, q) that maximize the objective function, which here is the power at ΔΠ1 within the power spectrum of the stretched period oscillation spectrum (see Section 2.3.1). Sequential iterations of TuRBO are shown from left to right. In each iteration, a region of (ΔΠ1, q) is uniformly sampled (dots), which forms the input to the Gaussian process component in TuRBO that provides a smooth and continuous approximation to the true parameter space. Here, lighter colors correspond to a larger power estimated at the corresponding ΔΠ1. The contours show the approximation of the Gaussian process to the entire 2D space, including regions outside the sampled space. As more iterations progress, the contour approximations become more detailed and accurate in modeling the whole 2D space. In each sampled region, x cand is determined as the optimal value from the approximation by the Gaussian process. Because the approximation is smooth and continuous, x cand is not restricted to follow any specific discretization of the parameter space. If x cand is the best solution across all current iterations (blue triangle), the search region in the next iteration is expanded about x cand. Otherwise, the search region is shrunk in the following iteration. Once the search region shrinks beyond a certain limit from consecutive failures in identifying a new global optimum, the search is reinitialized—here shown as Trial 2.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Distribution of ϵ  g  for the Kepler red giants in our study. The horizontal line indicates the asymptotic value of 0.22 predicted by Pinçon et al. (2019) in the weak coupling limit for stars early in their ascent of the red giant branch (RGB). Histograms are plotted separately for stars before and after 110 μHz in their evolution to highlight early RGB stars.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Same as Figure 7, but for bins of the stellar mass.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Observed mixed-mode rotational splitting δ ν rot for the 877 Kepler red giants in this study. The red line shows a fit of the form ﹩\delta {\nu }_{\mathrm{rot}}=k\cdot {{ \mathcal N }}^{a}﹩ to the data, with intervals indicating the 95% highest-density regions of the posterior predictive distribution. The histograms visualize a slight shift in the mean observed value of δ ν rot with evolution up the giant branch (increasing ﹩{ \mathcal N }﹩).
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Intercepts and gradients to the Δν–q relation from the posterior predictive samples, binned in metallicity (panels (a)–(b)) and stellar mass (panels (c)–(d)). The relation was fitted separately for mass and metallicity using hierarchical linear models, with the posterior distribution estimated using Markov Chain Monte Carlo techniques implemented in pymc3 (Salvatier et al. 2016).
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Metallicity dependence of the Δν−q sequence in our sample. Highlighted are seven new, metal-poor ([M/H] < −1.0 dex) Kepler targets not present in the Gehan et al. (2018) sample, with parameters tabulated in Table 2.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Replicated stretched period–power echelle diagrams for six stars from the Gehan et al. (2018) sample that show curvature in their g-mode pattern. These are (a) KIC 6786177, (b) KIC 6936091, (c) KIC 6953912, (d) KIC 7458743, (e) KIC 10973397, and (f ) KIC 11087371. Also shown are the peak-bagged dipole mixed-mode frequencies to guide the eye. The mixed-mode parameters to generate these diagrams are listed in Table 4. The construction of this diagram follows the implementation presented in Ong & Gehan (2023).
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Stretched period echelle diagram of KIC 3973247. The contours represent the 95% and 99% highest-density intervals of the BayesOpt samples in Figure 4, and indicate the uncertainty in the fit between the model and observed mixed modes.
Paper: Mixed-mode Ensemble Asteroseismology of Low-luminosity Kepler Red Giants
Authors: James S. Kuszlewicz, Marc Hon, Daniel Huber
Figure caption: Evolution of ϵ  g  for the stars in our sample as a function of the (a) metallicity and (b) mass.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Comparison of the HETDEX (HPSC-1) rest frame stack to stack of the classical LAE subset (26 out of 124) of KLCS with W  λ (Lyα) > 20 Å (Steidel et al. 2018; Pahl et al. 2021). The HPSC-1 stack has been corrected for IGM transmission, shifted by 250 km s−1 (Section 4.3), and converted to L  ν  units to match the KLCS data. Both spectra have been interpolated to the same wavelengths and smoothed with a 1 pixel (0.44 Å) Gaussian kernel (σ). The left-hand panel shows a section of the UV rest frame. The zoom-in insert shows the Lyman continuum region (shaded). The right-hand panel shows a zoom around the Lyα lines in velocity space relative to the assumed systemic redshift.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Stack from Figure 2 compared to a typical HPSC-1 LAE, ID: 2100541366 (R.A., decl.: 150.127594 +2.295267) to illustrate the S/N gains. This LAE is selected as it has properties similar to the sample average and ensemble: z = 2.566, g = 25.3, Lyα S/N = 5.9, Lyα log Luminosity = 42.81 (erg s−1), W  λ (Lyα) = 87 Å. The figure is cropped to the rest-frame wavelengths covered by the individual detection and aligned at Lyα. If we define the S/N simply as the ratio of the means of the flux and the errors on that flux (Gebhardt et al. 2021, and Section 4 in this work) between 1250 and 1650 Å, we see an improvement of more than 300× from the continuum S/N ≈ 0.06 in the individual detection to the S/N ≈ 21 in the stack.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Best-fitting, lowest-χ 2, FiCUS model (SB99 + SMC in Table 3). The black curve is the IGM corrected version of the full 50,000 stacked spectra shown in Figure 2 and the red curve denotes the FiCUS stellar continuum fit. Light gray regions, which correspond to most of the spectral features, are masked and not fit by the code. FiCUS is not designed to fit interstellar absorption or emission features.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Distribution of Lyα rest-frame equivalent widths in HPSC-1. The y-axis is normalized to the full 50,000 LAEs of this work. The black dashed vertical line marks the biweight location value of the distribution and the red dotted line the value as computed from the stack of the spectra. As most LAEs in HPSC-1 do not have detected continua, the individual equivalent widths are generally lower limits. The continuum in the stacked spectrum (Figure 2) is clearly detected and that computed equivalent width is more secure. See also Table 1.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Lyα luminosity in the HPSC-1 as functions of Lyα S/N and observed wavelength. The color, independently for each panel, tracks the number of galaxies. The highest luminosities occur at the lowest S/N and bluest wavelengths where the diminishing throughput of the instrument amplifies the scatter intrinsic to low S/N detections. The lower figure also shows a trend to larger luminosities with longer wavelengths; this is due to the HETDEX flux limits (Gebhardt et al. 2021) and is consistent with cosmological dimming.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Lyα rest-frame equivalent widths in HPSC-1 as functions of Lyα S/N and observed wavelength. The color, independently for each panel, tracks the number of galaxies. Since most HPSC-1 spectra do not have a detectable continuum, the equivalent widths are lower limits. There is an obvious loss of lower W  λ (Lyα) objects with increasing redshift, which is likely just the result of the HETDEX flux limits and cosmological dimming. The evidence for a true increase in equivalent width with redshift in this data set is very weak at best. See also Table 1.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: Normalized histograms of the 13,500 HPSC-1 LAEs in 2.9 < z < 3.5 and the 591 MUSE LAEs of the same redshift range (Kerutt et al. 2022). The distributions are similar, with 11% of these HETDEX LAEs and 16% of the MUSE LAEs exhibiting estimated W  λ (Lyα) values >240 Å and with biweight locations of W  λ (Lyα) values of 102.7 ± 80.2 and 85.4 ± 78.7 Å, respectively.
Paper: HETDEX Public Source Catalog 1—Stacking 50,000 Lyman Alpha Emitters 
Authors: Dustin Davis, Karl Gebhardt, Erin Mentuch Cooper, William P. Bowman, Barbara Garcia Castanheira, John Chisholm, Robin Ciardullo, Maximilian Fabricius, Daniel J. Farrow, Steven L. Finkelstein, Caryl Gronwall, Eric Gawiser, Gary J. Hill, Ulrich Hopp, Lindsay R. House, Donghui Jeong, Wolfram Kollatschny, Eiichiro Komatsu, Chenxu Liu, Maja Lujan Niemeyer, Alberto Saldana-Lopez, Shun Saito, Donald P. Schneider, Jan Snigula, Sarah Tuttle, Laurel H. Weiss, Lutz Wisotzki, Gregory Zeimann
Figure caption: The redshift distribution (mean z = 2.6) of the ∼50,000, flux-limited detection LAEs with Lyα S/N > 5.5 from HPSC-1.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: This plot shows the relationship between the age of the youngest detectable population, described in Section 4.2, and the stellar density, described in Section 2.4, where each point represents a cell. There seems to be a correlation between stellar density and the youngest ages detected, where the younger the stars in the cell are, the more dense that cell is. This correlation seems to flatten after 12 Myr.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Coadded SFHs of two regions of interest, the large H II region in the northeast spiral arm and the Hodge Complex, with the approximate locations of the regions used in the local SFH. The exact indices of the regions used in the SFH calculations are flagged in the machine-readable table.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Coadded SFRs across all spatial bins as a function of lookback time. The global SFR was much higher 16 Myr ago and has decreased to a steady rate in the past 10 Myr.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Left: best-fit foreground extinction A  V  of NGC 6946. Right: best-fit differential extinction dA  V  of NGC 6946.
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, 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, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: Significance map of the HAWC J1844−034 region with TeV γ-ray sources labeled at the top (H.E.S.S. Collaboration et al. 2018; Abeysekara et al. 2020; Albert et al. 2020; Cao et al. 2021; Amenomori et al. 2022), Fermi-LAT sources in red (Abdollahi et al. 2020), and known pulsars and SNR in green and blue, respectively (Bamba et al. 2001; Ueno et al. 2003; Manchester et al. 2005).
Paper: HAWC Study of the Very-high-energy γ-Ray Spectrum of HAWC J1844−034
Authors: A. Albert, C. Alvarez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, M. Breuhaus, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño de León, E. De la Fuente, D. Depaoli, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, V. Joshi, S. Kaufmann, J. Lee, H. León Vargas, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, L. Nellen, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, 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, E. Varela, L. Villaseñor, X. Wang, I. J. Watson, E. Willox, H. Zhou
Figure caption: The 1910 day HAWC significance map in Galactic coordinates highlighting the eHWC J1842−035 region. The brighter part of the map is the ROI used for the analysis. The labels indicate the known VHE γ-ray sources within the ROI. Note that 3HWC J1843−034 indicates the best-fit location of the source found from the HAWC all-energy catalog (Albert et al. 2020).