adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: CMDs for the GC/UCD populations in five massive galaxy clusters over a range of redshifts, drawing from recent JWST and HST measurements. They are arranged in order of age (reverse order of lookback time). Upper and lower dashed lines mark fiducial luminosity levels 107L⊙ and 108L⊙. The blue and red dots and lines in each panel mark the predicted luminosities of a 2 × 107M⊙ GC at two different metallicities (–2.0 and +0.2) and different ages appropriate for the given lookback time (see Table 2 and text). For each red/blue set of points the age increases from top to bottom. The decrease in luminosity from one panel to the next for these model lines is due only to direct stellar evolution, not accounting for any GC mass loss. Note that for the nearest object (NGC 4874 in the Coma cluster) the (F150W, F200W) magnitudes have been transformed from the HST optical bands (F475W, F814W); see text. NB: In A 2744 and RXJ2129, the thin sequences to the blue side of the GC/UCD sequence at a color index (F150W − F200W)0 ≃ −0.5 appear to be objects unassociated with the BCGs; see Paper I for discussion.
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: Left: the ambient CNM density and the scaled outflow radius inferred from equipartition analysis for multiple radio TDEs, taken from the literature. Also included are M87 and Sagittarius A*. Included as dotted and dashed lines are some example scaling relations. The thick black line is the density profile of AT2019azh constrained in this work. Empty points indicate observations with radio spectra with peaks that are not well constrained. Downward triangles for ASASSN-15oi indicate observations with only upper limits on the ambient density and lower limits on the radius. Right: the 5.5 GHz flux density and time since stellar disruption for a number of radio TDEs published in the literature. Data taken from C. T. Christy et al. (2024; ASASSN-19bt), A. J. Goodwin et al. (2022, 2023a, 2023b, 2025; AT2019azh, AT2020vwl, AT2020opy), Y. Cendes et al. (2021, 2022, 2024; AT2019dsg, AT2018hyz), K. D. Alexander et al. (2016; ASASSN-14li), A. Hajela et al. (2025; ASASSN-15oi), H. R. Russell et al. (2015; M87), F. K. Baganoff et al. (2003), and S. Gillessen et al. (2019; Sagittarius A*).
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: The 2.25, 5.5, 9, and 15.5 GHz light curve of AT2019azh. Empty markers are epochs previously presented in A. J. Goodwin et al. (2022), while filled markers are new observations presented in this work. The 15.5 GHz data are taken from I. Sfaradi et al. (2022).
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: Upper panel: model SEDs showing luminosity Lλ vs. wavelength for a SSP from E-MILES, at increasing redshifts. Lower panel: model SEDs now plotted as luminosity Lν vs. wavelength. Successive redshifts (from left to right) are z = 0.0, 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.8, 1.0, 1.3, 1.7, 2.0,  Each model curve has an age equal to (12 − TL(z)) Gyr where TL(z) is the lookback time corresponding to z. These curves may be used to gauge the wavelength range and thus the filters across which the detected signal from the GC is maximal.
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: Individual frequency light-curve fits for the Sedov–Taylor model generated by MCMC modeling using Equation (4). The range of fits is broadly consistent with the observed flux densities but with some deviation due to more structured light curves at 9 and 11 GHz.
Paper: JWST Photometry of Globular Cluster Populations in MACS0417.5−1154
Authors: William E. Harris, Marta Reina-Campos, Kaitlyn E. Keatley, Maruša Bradač, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Ghassan T. E. Sarrouh, Marcin Sawicki, Chris J. Willott, Samantha C. Berek
Figure caption: Top panel: radial distribution of point sources around the BCG. Objects in the bluer and redder halves of the CMD in (F115W − F200W) are plotted separately. Lower panel: azimuthal distribution in 20° sectors, again separately for the bluer and redder GC subsets.
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: Expected evolution of the 1.39 GHz radio emission of AT2019azh assuming the Sedov–Taylor decay model (blue line) and the observed 1.39 GHz flux densities of AT2019azh to date (black points). Included are the 3σ sensitivities of the VLA-C configuration and SKA-Mid band 2 (0.95–1.76 GHz) for a 1 hr observation, as well a 1.4 GHz upper limit of the host galaxy emission from archival FIRST (R. H. Becker et al. 1995).
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: MCMC spectral fits of the radio observations (scatter points) using Equation (1) are given by the solid lines. The peak frequency is not well constrained for a majority of the epochs due to a lack of data at low frequencies. Δt is time since the launch of the outflow.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Summary lightcurves of the AU Mic X-ray campaign that overlap with the SMARTS/CHIRON spectroscopic data (2018 October 10–25). (a) and (b) Hα and Hβ equivalent width (E.W.) values from the SMARTS/CHIRON spectroscopic data with the time cadence of 65 s. Gray numbers (in (a)) and gray dashed lines (in all the panels) show Hα flares and their timings, respectively, which are identified in T23 (see Table 6 of T23). (c) and (d) XMM EPIC-pn X-ray (0.2–12 keV) and XMM OM UVW2 data are plotted in units of counts per second, and with 30 and 10 s binnings, respectively. Flares 11 and 15, which are discussed in detail in Section 4.2, are marked with the gray numbers in (c). (e) and (f) LCOGT U-band and SMARTS V-band photometric data are plotted in relative flux units, and with the time cadence of 46 and 47 s, respectively. (g) VLA Ku-band data in the unit of flux density (mJy) and with the time binning of 10 s (from T25).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) XMM EPIC-pn X-ray (0.2–12 keV) lightcurve of AU Mic for the data period of Obs-ID 0822740301 (2018 October 10 13:13:59.760 to 2018 October 12 01:42:19.177 UTC), plotted in units of counts per second, and with 30 s binning. The red numbers show flares identified by T23, and the start, peak, and end times of these flares (from Table 6 of T23) are shown with green and orange colored regions. (b) Same as (a) but for the EPIC-MOS1 (0.2–12 keV) lightcurve and the combined one of RGS1 and RGS2 data. (c) and (d) XMM OM UVW2, LCOGT U-band, and VLA Ku-band lightcurves as in Figures 1(d)–(g), but for the data period of the X-ray data in (a) and (b). The flare peak times in the XMM X-ray data (in (a)) are also plotted as gray dashed lines in (c) and (d).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 3, but for the period of the XMM X-ray data Obs-ID 0822740601 (2018 October 16 23:39:21.362 to 2018 October 17 18:17:33.004 UTC ). No overlapping VLA Ku-band data exist here (see Figure 1).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) Hα and Hβ equivalent width (E.W.) lightcurves as in Figures 1(a) and (b), but for the data of 2018 October 13 and 14, which overlap with the X-ray data in (b) and (c). (b) and (c) The X-ray lightcurve data as inn Figures 2(a) and (b) but for Obs-ID 0822740401 (2018 October 12 13:06:33.808 to 2018 October 14 01:36:22.232 UTC). (d),(e), and (f) XMM OM UVW2, LCOGT U-band and SMARTS V-band ,and VLA Ku-band lightcurves as in Figures 1(d)–(g) and 2(c) and (d), but for the data period of the X-ray data in (b) and (c).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 3, but for the period of the XMM X-ray data Obs-ID 0822740501 (2018 October 14 12:21:18.787 to 2018 October 16 00:04:00.273 UTC).
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: Comparison of measured AT2019azh flux density with measured flux density of a background source in the image field at 1.65, 5.5, and 9 GHz. Black stars are AT2019azh data, and blue dots are the background source.
Paper: The 6 yr Radio Light Curve of the Tidal Disruption Event AT2019azh
Authors: M. Burn, A. J. Goodwin, G. E. Anderson, J. C. A. Miller-Jones, Y. Cendes, C. Christy, W. Lu, S. van Velzen
Figure caption: Simple power law and astropy SMOOTHLYBROKENPOWERLAW1D function fit to 1443 days spectra.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Hα, Hβ, and LCOGT U-band lightcurves of 2018 October 18, 19, and 20. The flares identified in Hα data by T23 are shown with pink colored regions, which correspond to the start and end times of these flares (from Table 6 of T23).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) XMM EPIC-pn X-ray (0.2–12 keV) and XMM OM UVW2 lightcurves around Flares 11 and 15 (see Figure 2). (b) XMM EPIC-pn and EPIC-MOS1 X-ray lightcurves (0.2–12 keV) of Flares 11 and 15. The green and pink colored regions correspond to the Phases 1–10, separated for the spectral analysis. (c)–(e) The spectral analysis results (X-ray luminosity in 0.2–12 keV LX, temperature T, and emission measure EM) of Phases 1–11 of Flares 11 and 15 (from Table 6).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 15 but for the Hβ line.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Multiwavelength lightcurves around Flares 35–37 (enlarged lightcurve of Figure 4). (a) XMM EPIC-pn X-ray (0.2–12 keV) lightcurve. The rise and decay phases of Flares 35–37 are shown with green and yellow colored regions (see Figure 4). The preflare phase and the potential dimming phase (separated into (i) and (ii); see A. M. Veronig et al. 2021) are also shown with gray, cyan, and pink colored regions. (b) XMM EPIC-MOS1 X-ray (0.2–12 keV) lightcurve. (c) Hα and Hβ equivalent width (E.W.) values. The gray and pink colored regions correspond to time [1]–[4], whose spectra are shown in Figure 20. (d) and (e) LCOGT U-band, SMARTS V-band, and VLA Ku-band lightcurves. The vertical gray dashed lines show peak times of VLA Ku-band radio flares identified in T25.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) and (c) The Hα and Hβ E.W. lightcurves of Flare 65 on 2018 October 24 are plotted with red circles and blue marks. (b) Time evolution of the Hα profile from the CHIRON spectra. The vertical axis represents the wavelength, while the gray horizontal dashed lines with velocity values represent the Doppler velocities from the Hα line center. The gray vertical dashed lines indicate the time [1] to time [6], which are shown in (a) (lightcurve) and Figure 43 (spectra). The color map represents the line profile changes from the quiescent profile (see Figures 43(b), (f), and (j)). (c) and (d) Same as panels (a) and (b), but for the Hβ line. (e) and (f) Same as panels (a) and (b), but for He I D3 5876 Å line and Na I D1 and D2 lines. (g) and (h) Same as panels (a) and (b), but for the Ca II 8542 Å line. The excess equivalent width values of Na I D1 and D2 and Ca II 8542 lines are plotted in (e) and (g).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) and (b) Hα and Hβ equivalent width (E.W.) lightcurves as plotted in Figure 1. The flare times (based on the start and end times from T23) are shown with gray points to show quiescent phase modulations. (b) XMM EPIC-pn X-ray lightcurve as plotted in Figure 1, but enlarged in the y-axis direction. (c) TESS lightcurve of AU Mic Cycle 1 taken from Figure 1(a) of K. Ikuta et al. (2023), but shifted along the x-axis direction with 13 × 4.863 days (13 × AU Mic’s rotation period).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) Line profiles of the Hα emission line during Flare 35 on 2018 October 15 from the CHIRON spectra. The horizontal and vertical axes represent the wavelength and flux normalized by the continuum. The gray vertical dashed lines with velocity values represent the Doppler velocities from the Hα line center. The red solid and blue dashed lines indicate the line profiles at the time [1] and time [2], respectively, which are indicated in Figure 18(c) (lightcurve) and are during Flare 35. The black dotted line indicates the line profiles in quiescent phase, which are the average profile during −0.19 to +0.89 hr on this date (see Figure 18(c)). (e) Same as panel (a), but the line profiles at time [3] and time [4] during Flares 35 and 36, respectively. (c) and (g) Same as (a) and (e), but for the Hβ emission line. (b), (d), (f), and (h) Same as panels (a), (c), (e), and (g), respectively, but the line profile differences from the quiescent phase.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: EMtot–Tobs relation. Red filled circles show EMtot and Tave values of AU Mic estimated in this study (Table 1). Blue open diamonds and black filled squares indicate the data of G dwarfs and the solar maximum/minimum, respectively, and they are taken from Figure 5 of S. Takasao et al. (2020). (a) Gray dotted and green dashed lines show Equations (1) and (2) with different parameters. (b) Data points with Equation (4) with different values of N0, f = 0.1, ﹩\bar{B}=100﹩ G, and Fh = 107erg cm−2 s−1 (see the main text for the details).
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Cumulative distribution of volume and distance for BNS (top) and NSBH (bottom) events at 90% credible intervals for the three simulations using the same color scheme as in Figure 1. The median distance or volume for each configuration is annotated in the respective panel.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Cumulative distribution of sky localization area at 50%, 70%, and 90% credible intervals for simulations 1 (black line), 2 (red line), and 3 (blue line) for BNS (top) and NSBH (bottom) events. The median localization area for each configuration is annotated in the respective panel.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Chirp mass vs. luminosity distance for BNS (left) and NSBH (right) events in the O5 simulation. The yellow squares represent all BNS/NSBH events detected in GWs; the cyan squares show all mergers for which a KN is produced according to our model and fiducial EOS. Out of all the KNe, those with a black point and/or a red circle were detected in g and/or i band, respectively. The same color scheme applies to the histograms. We limit the plot to a chirp mass of 3.5 M⊙ for the NSBH merger since no KN is produced beyond this chirp mass in our simulations. For both cases, the lower chirp mass end of the distribution yields higher KN detection rates than at higher mass.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Total ejected mass from BNS mergers vs. their total mass. Vertical dashed lines delineate between different merger remnants’ fates, with the threshold masses and radii derived assuming the EOS from S. Huth et al. (2022b). Here MTOV = 2.436 M⊙, RTOV = 11.7 km, and Mth = 3.616 M⊙. The color scheme is the same as in Figure 4, except that by construction we do not have BNSs that do not produce a KN here. The pink and yellow lines indicate the fate of GW170817 and GW190425 remnants according to our assumptions.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Component masses of BNS (left) and NSBH (right) systems and their effect on KN detection. We limit m1 to ﹩{8}_{{M}_{\odot }}﹩ in the plot for visualization purposes. The color scheme is the same as in Figure 4.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Mass ratio vs. chirp mass for the BNS merger events (left panel) and NSBH mergers (right panel) from the O5 simulation. The color scheme is the same as in Figure 4.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Viewing angle of the BNS (left) and the NSBH (right) mergers vs. their distance for the O5 simulations. The color scheme is the same as in Figure 4.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Effective spin χeff vs. luminosity distance for our O5 simulated NSBH mergers. The color scheme is the same as in Figure 4.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: 90% C I area vs. luminosity distance for BNS (top) and NSBH (bottom) events with the same color scheme as in Figure 1.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: Simulated DECam tiling follow-up of a well-localized BNS event. The solid and dashed lines indicate the 50% and 90% C I area of the event, respectively. It can be seen that the 90% probability region of the event is covered almost entirely by DECam with ∼15 pointings.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: BNS KN magnitude distributions at 0.5, 1, 2 and 4 days as a function of chirp mass bins. The top panel shows the results in g band; the bottom panel shows the results in i band.
Paper: Detecting Electromagnetic Counterparts to LIGO/Virgo/KAGRA Gravitational-wave Events with DECam: Neutron Star Mergers
Authors: K. Kunnumkai, A. Palmese, A. M. Farah, M. Bulla, T. Dietrich, P. T. H. Pang, S. Anand, I. Andreoni, T. Cabrera, B. O'Connor
Figure caption: NSBH KN magnitude distributions at 0.5, 1, 2 and 4 days as a function of chirp mass bins. The top panel shows the results in g band; the bottom panel shows the results in i band.