adsabs/AstroCLIMB huggingface dataset:
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Effective optical flux limit (﹩{f}_{\mathrm{eff},\mathrm{opt}}={f}_{\mathrm{opt}}{T}_{\exp }/{t}_{\mathrm{opt}}﹩) to radio flux ratio with respect to the optical burst duration (t opt), color-coded by the exposure time (﹩{T}_{\exp }﹩), for the sample of FRBs with simultaneous optical observations (including the nearly simultaneous Binospec observation for FRB 20220912A). The quoted magnitude limits are the extinction-corrected values for each FRB, and their solid lines extend from the time of radio burst to the end of each exposure. The dotted extension to the nearly simultaneous Binospec observation shows f eff,opt within the timing uncertainty. The shaded regions show the flux error ranges of the Galactic SGR 1935+2154 due to the large extinction uncertainty. Broad ranges of optical burst model predictions from Yang et al. (2019) are also plotted as rectangular regions, where the duration of one-zone models are shown with a width corresponding to the mean plus one standard deviation of the t FRB distribution of each FRB. Potential constraints from future observations with Subaru HSSC are also plotted as dashed lines for each FRB. Note that the optical limits of FRBs 20121102A and 20190520Bs barely reach the pulsar nebula model parameter space, while our limits for FRB 20200912A and published limit for SGR 1935+2154 reach the pulsar magnetosphere as well as the pulsar nebula model parameter spaces.
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Ratio of optical flux limit (in janskys; in the g, c, r, o, i, and z bands from the top to bottom rows) to radio fluence (in janskys times millisecond) with respect to the temporally closest FRB detection for our sample of eight repeating FRBs (including the Galactic SGR 1935+2154); labels are as in Figure 2. In the case when the radio fluence of a particular burst is not available, it is assumed to be the mean of the fluence distribution of that particular repeating FRB (and shown as a transparent point with an upper error bar corresponding to one standard deviation). The dashed and dotted gray lines in each panel show F opt/F radio = 1, 0.1, 0.01, and 0.001, assuming F opt = f opt × Δt, where Δt is the time delay between the optical and radio observations. Note that most of the simultaneous observations (KeplerCam, LCO, TNT, MAGIC, Tome-e, BOOTES), targeted Binospec and APO, and some untargeted ZTF observations are in the regime of F opt/F radio ≲ 1. Our KeplerCam and LCO limits for FRB 20220912A are comparable even to the BOOTES simultaneous observation of SGR 1935+2154 (f opt/F radio ≲ 10−7 ms−1, or F opt/F radio ≲ 10−3). Our nearly simultaneous Binospec limit is at f opt/F radio ≲ 10−8 ms−1, or F opt/F radio ≲ 10−4 at Δt ≈ 0.4 s.
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: FRB-based estimates (points) and optical-based constraints (shaded regions) on the external density (n ext) and flare energy (﹩{E}_{\mathrm{flare}}﹩) in the synchrotron maser model (Figure B1). The contours mark the number of most stringent optical limits (i.e., deeper limits with shorter delays; from left to right in each panel: 1, 5, 25, 50, 100, and 200) used to constrain the parameter space, while the gray dashed and dotted lines show the possible constraints from future observations: 60–300 s exposures (limiting magnitude of 20–22) with 1–5 minutes delay using a 1 m class telescope (e.g., KeplerCam and LCO), and simultaneous 0.1–1 s exposure (limiting magnitude of 20–22) using an 8 m class telescope (e.g., Subaru HSSC). Note that optical limits already reach the high-﹩{E}_{\mathrm{flare}}﹩ ends of the distributions for FRB 20180916B and SGR 1935+2154, and down to the mid-﹩{E}_{\mathrm{flare}}﹩ range (≈65%) of the distribution of FRB 20220912A with our KeplerCam, LCO, and Binospec observations. The future observations have potential to reach FRBs 20200120E and FRB 20201124A, and to constrain SGR 1935+2154 even further.
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Frequency and luminosity evolution (in the r band) of the synchrotron maser model (Metzger et al. 2019; Margalit et al. 2020a, 2020b) with an FRB duration t FRB = 1 ms, assuming a shell-like density distribution and fractional magnetization σ = 0.3 (see Equations (B1)–(B5)). The light curves exhibit changing evolution in each frequency regime (ν  r  < ν cool, ν cool < ν  r  < ν syn, and ν syn < ν  r ). Left: models with a fixed density of n ext = 2000 cm−3, color-coded by ﹩{E}_{\mathrm{flare}}﹩. Right: models with a fixed flare energy of ﹩{E}_{\mathrm{flare}}={10}^{46}﹩ erg, color-coded by n ext.
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Top: schematic timeline of the KeplerCam and LCO simultaneous exposures, as well as the temporally closest MMT/Binospec exposure with respect to the FRB 20220912A bursts detected by CHIME and DSA (where N is the number of bursts detected within 1 s), color-coded by the observed r-band limiting magnitude. The UT date labeled next to each point is its exposure start time. In total, we covered 13 bursts in 10 simultaneous exposures: one DSA detection each in two KeplerCam exposures, one CHIME detection each in five KeplerCam exposures, and two CHIME detections each in two KeplerCam and one LCO exposures. Bottom: simultaneous KeplerCam 60 s image during the two CHIME detections (left), the corresponding PS1 template image (middle), and the resulting difference image (right), with the DSA localization region and host galaxy marked by the magenta ellipse (ΔR.A. ∼ 2″ and Δdecl. ∼ 1″; Ravi et al. 2022a) and navy circle (Kron radius =3.″44 from PS1 DR2; Flewelling et al. 2020), respectively. No optical counterpart is identified down to a r-band limiting magnitude of 21.1.
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Same as Figure 2, but for the non-repeating FRBs (summarized in Table A1). Note the much less constraining luminosity and temporal ranges, compared to those of the repeating FRBs, given the small number of bursts and their large distances. Optical data sources: LCO (Núñez et al. 2021 for FRBs 20190608B and 20190714A in the r band), ZTF forced-photometry service (Masci et al. 2019 and this work for all the FRBs), ATLAS forced photometry server (Shingles et al. 2021 and this work for all the FRBs).(The data used to create this figure are available.)
Paper: Limits on Simultaneous and Delayed Optical Emission from Well-localized Fast Radio Bursts
Authors: Daichi Hiramatsu, Edo Berger, Brian D. Metzger, Sebastian Gomez, Allyson Bieryla, Iair Arcavi, D. Andrew Howell, Ryan Mckinven, Nozomu Tominaga
Figure caption: Same as Figure 3, but for the non-repeating FRBs. Note that all available observations are in F opt/F radio ≳ 1 regime.
Paper: Early Results from GLASS-JWST. XV. Properties of the Faintest Red Sources in the NIRCAM Deep Fields
Authors: K. Glazebrook, T. Nanayakkara, C. Jacobs, N. Leethochawalit, A. Calabrò, A. Bonchi, M. Castellano, A. Fontana, C. Mason, E. Merlin, T. Morishita, D. Paris, M. Trenti, T. Treu, P. Santini, X. Wang, K. Boyett, Marusa Bradac, G. Brammer, T. Jones, D. Marchesini, M. Nonino, B. Vulcani
Figure caption: Image montages and Prospector SED fits of example objects. As well as the 						individual bands we show a “wide” RGB color image constructed from F444W, 						F356W, and F200W. The black points in the SED plots show the observed 						photometry with the larger symbols being the GLASS NIRCAM bands; the red 						line shows the best SED from Prospector. The colored text shows the 						corresponding BLUE_BRIGHT and RED_BRIGHT magnitudes. The large red points 						are photometry of the best-fit SED and the legend shows the physical 						parameter’s 68% range. p(z) probability distributions are shown for the SED fits in the 						right panels with vertical lines denoting best-fit redshifts and 						uncertainties. In the top plot the NIRCAM filter transmission profiles are 						plotted to show their extent. ID14903 agrees much better with an ultracool 						stellar template (shown as the orange curve) rather than a high-redshift 						galaxy. We show in the bottom two panels two z 						> 11 Lyman break galaxy candidates. ID22600 is a strong candidate 						(Castellano et al. 2022); 						ID12761 is a poor candidate and likely contaminated despite the strongly 						peaked p(z).
Paper: Early Results from GLASS-JWST. XV. Properties of the Faintest Red Sources in the NIRCAM Deep Fields
Authors: K. Glazebrook, T. Nanayakkara, C. Jacobs, N. Leethochawalit, A. Calabrò, A. Bonchi, M. Castellano, A. Fontana, C. Mason, E. Merlin, T. Morishita, D. Paris, M. Trenti, T. Treu, P. Santini, X. Wang, K. Boyett, Marusa Bradac, G. Brammer, T. Jones, D. Marchesini, M. Nonino, B. Vulcani
Figure caption: Redshift–magnitude distribution of the BLUE_BRIGHT−RED_BRIGHT >1 selected 						sources. Vertical bars denote the redshift uncertainty. Symbol size and 						color are keyed to stellar mass, spectral type (quiescent/star-forming), and 						dust attenuation as given in the legend. Open circles are the same coding, 						but denote objects that would be undetected in F160W in a deep HST survey, 						while the dashed vertical line shows the approximate Spitzer confusion 						limit.
Paper: Early Results from GLASS-JWST. XV. Properties of the Faintest Red Sources in the NIRCAM Deep Fields
Authors: K. Glazebrook, T. Nanayakkara, C. Jacobs, N. Leethochawalit, A. Calabrò, A. Bonchi, M. Castellano, A. Fontana, C. Mason, E. Merlin, T. Morishita, D. Paris, M. Trenti, T. Treu, P. Santini, X. Wang, K. Boyett, Marusa Bradac, G. Brammer, T. Jones, D. Marchesini, M. Nonino, B. Vulcani
Figure caption: Photometrically inferred emission line (Hβ + [O 							III] 4961,5007 Å) equivalent widths and rest-frame ultraviolet 							β values for objects in our selected 						sample with RED_BRIGHT > 25 and 2 < z 						< 6.
Paper: Conclusive Evidence for a Population of Water Worlds around M Dwarfs Remains Elusive
Authors: James G. Rogers, Hilke E. Schlichting, James E. Owen
Figure caption: Synthetic mass–radius distributions are shown for populations of planets evolved with photoevaporation and core-powered mass loss in left- and right-hand panels, respectively, colored by their equilibrium temperatures. Super-Earths are stripped of their H/He-dominated atmospheres and fall onto a relation consistent with an Earth-like composition (brown dashed line), while sub-Neptunes retain a significant atmosphere. In the top panels, we assume an initial distribution of atmospheric masses appropriate for a boil-off scenario (Equation (2)), in which planets lose a significant amount of H/He mass during disk dispersal. We characterize the resulting narrow mass–radius distribution with a median line (orange dashed line; Equation (5)). In the middle panels, we adopt agnostic initial conditions (Equation (3)) and parameterize this mass–radius relation with 2σ limits (orange dotted lines). In the bottom panels, we compare our theoretical mass–radius distributions (orange dashed and dotted lines; Equation (5)) with the observed sample of M-dwarf orbiting exoplanets from Luque & Pallé (2022), together with the mass–radius relation for water worlds (blue solid line; Equation (1)). We find that boil-off initial conditions provide mass–radius relations that are completely degenerate with that of water worlds. Furthermore, even when adopting agnostic initial conditions, the observations are accurately reproduced since the mass–radius distribution is naturally explained due to mass loss and cooling/contraction of H/He-dominated atmospheres. We highlight planets with confirmed escaping H/He detections with blue-shaded regions (namely, K2 18 b, GJ 3470 b, GJ 436 b, and, tentatively, GJ 1214 b).
Paper: Conclusive Evidence for a Population of Water Worlds around M Dwarfs Remains Elusive
Authors: James G. Rogers, Hilke E. Schlichting, James E. Owen
Figure caption: The final atmospheric mass fractions (left-hand column) and planet radii (right-hand column) after 5 Gyr of photoevaporative evolution for populations of planets with equilibrium temperatures of 300 ± 10 K (top row), 500 ± 10 K (middle row), and 800 ± 10 K (bottom row). Colors for points represent planet size in the left-hand panels and final atmospheric mass fraction in the right-hand panels, demonstrating that larger atmospheric mass fractions lead to larger planets and vice versa. All planets start their evolution with an initial distribution of atmospheric mass fractions (displayed as gray line) that account for gaseous core accretion and boil-off during protoplanetary disk dispersal (see Equation (2)). To corroborate these semianalytic results, we also perform numerical models with MESA, which are shown as black triangles. In general, sub-Neptunes only exist at larger masses for higher equilibrium temperatures. The mass–radius distribution (as seen in Figure 1) is a superposition of all equilibrium temperatures. In the right-hand column, we compare our mass–radius distributions with the models of Lopez & Fortney (2014) in blue and Zeng et al. (2019) in black for atmospheric mass fractions of 0.1% and 1.0%. We highlight that the models of Zeng et al. (2019) assume constant specific entropy defined with a temperature at fixed pressure at 100 bars (not to be confused with the equilibrium temperature) and therefore suggest a dramatic increase in planet radius for lower-mass planets. The models of Lopez & Fortney (2014) consider irradiation and cooling for planets with constant atmospheric mass fraction, meaning they are more appropriate for analysis of planet composition. Our mass–radius models account for loss-induced scaling of atmospheric mass with planet mass, meaning they are appropriate for comparisons of planet populations in the mass–radius diagram.
Paper: Solar System-scale Interferometry on Fast Radio Bursts Could Measure Cosmic Distances with Subpercent Precision
Authors: Kyle Boone, Matthew McQuinn
Figure caption: The triangular configuration of two detectors and the source used for timing.
Paper: Solar System-scale Interferometry on Fast Radio Bursts Could Measure Cosmic Distances with Subpercent Precision
Authors: Kyle Boone, Matthew McQuinn
Figure caption: Example of a detector configuration that can be used to measure the distance to a source from the curvature of its wave front. The signal will arrive at detector B before it is seen at detectors A or C. By comparing the arrival times at the three detectors we can infer the distance to the source. Note that we can only measure the difference in arrival times, not the distances d  i  directly. With two detectors the distance to the source is degenerate with the angular position on the sky θ. With three detectors in two dimensions, or four detectors in three dimensions, this degeneracy is broken and the distance to the source can be inferred.
Paper: Solar System-scale Interferometry on Fast Radio Bursts Could Measure Cosmic Distances with Subpercent Precision
Authors: Kyle Boone, Matthew McQuinn
Figure caption: Time delays vs. projected baseline length x ⊥ for ν = 4 GHz (top panel) and ν = 8 GHz (bottom panel). The solid lines are the cosmological delay owing to wave front curvature, Δt  d , for d = 100 Mpc (blue) and d = 1000 Mpc (red). The other lines are estimates for different systematics: the differential dispersion from the Galaxy (Equation (14) assuming SM ﹩\equiv \,{C}_{n}^{2}L={10}^{-4}\,\mathrm{kpc}\,{{\rm{m}}}^{-20/3}﹩), the scattering time (taken to be ﹩{\sigma }_{t}^{\mathrm{sc}}=50\,\mathrm{ns}\,{[\nu /1\,\mathrm{GHz}]}^{-4}﹩, 2× larger than the mean NE2001 model at b = 90°; Equation (12)), the Shapiro time delay for d = 103 Mpc (assuming the cosmological delay is dominant; Equation (D4)), and the VLBI group delay timing error (assuming S/N = 5 and Δν = 0.2 ν; Equation (11)). Even though it is often larger than the signal Δt  d , differential dispersion can be removed using its frequency dependence (Section 4.2). The baselines over which the solid lines representing Δt  d  are thickest show where VLBI timing and scattering delays (all calculated in the manner described above) are each <3% of Δt  d . Shapiro delays, if not removed using their quadrupolar shape, limit <3% precision to d ≲ 103 Mpc.
Paper: Solar System-scale Interferometry on Fast Radio Bursts Could Measure Cosmic Distances with Subpercent Precision
Authors: Kyle Boone, Matthew McQuinn
Figure caption: Estimated fractional distance error, σ  d /d, to a single FRB as a function of distance d, for observations at ν = 4 GHz (top panel) and ν = 8 GHz (bottom panel). The different colors indicate different detector separations x ⊥: 12.5 au in brown, 25 au in orange, 50 au in green, 100 au in red, and 200 au in purple. The solid curves assume to compute the timing error (σ  t ) , that each baseline vector is constrained to a 1σ error of δ x = 3 cm in the top and δ x = 1 cm in the bottom panel, an error which includes the VLBI timing error, in addition to including the noise from scattering and Shapiro time delays assuming the same specifications as used in Figure 3. The highlighted regions show how these uncertainties change over the specified range of δ x. The dashed curves, only shown for the three longest baselines, are the same but assume the Shapiro delay is removed owing to its different angular dependence. The dotted curve is the fractional redshift uncertainty that arises if the peculiar velocity can be corrected for using large-scale structure observations to 200 km s−1. The vertical lines show the comoving light-travel distance that corresponds to redshifts of z = 0.05, 0.5, and 5 in a flat ΛCDM cosmology with Ω M  = 0.3 and h = 0.7.
Paper: Early Results from GLASS-JWST. XIV. A Spectroscopically Confirmed Protocluster 650 Million Years after the Big Bang
Authors: Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Gabriel Brammer, Charlotte A. Mason, Michele Trenti, Benedetta Vulcani, Xin Wang, Ana Acebron, Yannick Bahé, Pietro Bergamini, Kristan Boyett, Marusa Bradac, Antonello Calabrò, Marco Castellano, Wenlei Chen, Gabriella De Lucia, Alexei V. Filippenko, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Patrick L. Kelly, Anton M. Koekemoer, Nicha Leethochawalit, Ting-Yi Lu, Danilo Marchesini, Sara Mascia, Amata Mercurio, Emiliano Merlin, Benjamin Metha, Themiya Nanayakkara, Mario Nonino, Diego Paris, Laura Pentericci, Piero Rosati, Paola Santini, Victoria Strait, Eros Vanzella, Rogier A. Windhorst, Lizhi Xie
Figure caption: NIRSpec spectra in the observed wavelength frame (PRISM for the top four and G395H grating for the bottom three) of the confirmed protocluster members. For each galaxy, the top panel shows the 2D and 1D full spectrum, where the position of Lyman break, Hβ line, and [O III] doublets are indicated (blue vertical lines); the bottom left panel shows a zoomed region around the Lyman break, along with a best-fit template by gsf (cyan), where the detector gap region in the G140H grating is masked (gray); the bottom right panel shows the continuum-subtracted spectrum in the region of the Hβ+[O III]-doublet lines, where lines with >5σ detection are hatched in yellow. For YD4, where both PRISM and G395H spectra available, the latter is shown. The fitted three-component Gaussian model is also shown (blue). It is noted that the 1D full spectrum in the top panel is resampled to a coarse spectral grid for visualization purposes.
Paper: Early Results from GLASS-JWST. XIV. A Spectroscopically Confirmed Protocluster 650 Million Years after the Big Bang
Authors: Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Gabriel Brammer, Charlotte A. Mason, Michele Trenti, Benedetta Vulcani, Xin Wang, Ana Acebron, Yannick Bahé, Pietro Bergamini, Kristan Boyett, Marusa Bradac, Antonello Calabrò, Marco Castellano, Wenlei Chen, Gabriella De Lucia, Alexei V. Filippenko, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Patrick L. Kelly, Anton M. Koekemoer, Nicha Leethochawalit, Ting-Yi Lu, Danilo Marchesini, Sara Mascia, Amata Mercurio, Emiliano Merlin, Benjamin Metha, Themiya Nanayakkara, Mario Nonino, Diego Paris, Laura Pentericci, Piero Rosati, Paola Santini, Victoria Strait, Eros Vanzella, Rogier A. Windhorst, Lizhi Xie
Figure caption: A 5.″4 × 5.″4 smoothed F200W NIRCam image centered on YD4, with slits from various programs overlayed. The ∼0.″2 × 1.″2 NIRSpec/MSA slits from GLASS and the DDT are shown in red and cyan, respectively, while the ∼0.″9 × 11″ VLT/X-Shooter long-slit from (Laporte et al. 2017) is shown in yellow. The two NIRSpec slits clearly isolate YD4 from a nearby, fainter companion ∼0.″5 southeast of its position (YD6); however the X-Shooter long-slit includes both objects, as well as YD7 located to its west.
Paper: Early Results from GLASS-JWST. XIV. A Spectroscopically Confirmed Protocluster 650 Million Years after the Big Bang
Authors: Takahiro Morishita, Guido Roberts-Borsani, Tommaso Treu, Gabriel Brammer, Charlotte A. Mason, Michele Trenti, Benedetta Vulcani, Xin Wang, Ana Acebron, Yannick Bahé, Pietro Bergamini, Kristan Boyett, Marusa Bradac, Antonello Calabrò, Marco Castellano, Wenlei Chen, Gabriella De Lucia, Alexei V. Filippenko, Adriano Fontana, Karl Glazebrook, Claudio Grillo, Alaina Henry, Tucker Jones, Patrick L. Kelly, Anton M. Koekemoer, Nicha Leethochawalit, Ting-Yi Lu, Danilo Marchesini, Sara Mascia, Amata Mercurio, Emiliano Merlin, Benjamin Metha, Themiya Nanayakkara, Mario Nonino, Diego Paris, Laura Pentericci, Piero Rosati, Paola Santini, Victoria Strait, Eros Vanzella, Rogier A. Windhorst, Lizhi Xie
Figure caption: NIRCam red giant branch composite image of the Abell 2744 field (blue, F115W; green, F200W; red, F444W). Confirmed galaxies are marked by red squares and shown individually in the zoomed-in panels (2.″2 × 2.″2). The position of the micro‐shutter assembly (MSA) slit for each object is shown a rectangle (colored in cyan for the Director's Discretionary Time (DDT) program and red for the GLASS-ERS). The remaining photometric z ∼ 7.9 candidates that were originally identified in Zheng et al. (2014) but not covered by our NIRSpec observations are marked in orange circles.