adsabs/AstroCLIMB huggingface dataset:
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: The 2000 × 2000 pixel subimage of GB110, one of the most densely populated stellar fields, with 8.58 s exposure.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: The distribution of the observed PSF FWHMs in the H-band images over approximately 14 months. The median is 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩33 (red line), and the mode is 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩20 (blue line).
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: The slope images of the microlensing events PRIME-2024-BLG-124 (top panels) and 170 (bottom panels) before (left) and after (right) DIA processing with 50″ × 50″ (100 × 100 pixels). The targets are marked with a green cross.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: The light curve of the binary event PRIME-2024-BLG-066, detected in field GB92. The vertical axis shows the differential flux (Δflux) in ADU. The best-fit parameters are the mass ratio q = 0.139 ± 0.019, separation s = 1.531 ± 0.076, and event timescale tE = 21.8 ± 2.9 days.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: Same as Figure 5 but for new observational fields of PRIME toward the GB since 2025 June 2. The red, yellow, blue and cyan squares represent fields with cadences of 21.6 minutes, 43.1 minutes, 86.2 minutes and 1 day, respectively.
Paper: The PRime-focus Infrared Microlensing Experiment (PRIME): First Results
Authors: Takahiro Sumi, David A. H. Buckley, Alexander S. Kutyrev, Motohide Tamura, David P. Bennett, Ian A. Bond, Giuseppe Cataldo, Joseph M. Durbak, S. Bradley Cenko, Dale Fixsen, Orion Guiffreda, Ryusei Hamada, Yuki Hirao, Asahi Idei, Dan Kelly, Markus Loose, Gennadiy N. Lotkin, Eric I. Lyness, Stephen Maher, Shuma Makida, Noriyuki Matsunaga, Shota Miyazaki, Gregory Mosby, Samuel H. Moseley, Tutumi Nagai, Togo Nagano, Seiya Nakayama, Mayu Nishio, Kansuke Nunota, Ryo Ogawa, Ryunosuke Oishi, Yui Okumoto, Nicholas J. Rattenbury, Yuki K. Satoh, Elmer H. Sharp, Daisuke Suzuki, Takuto Tamaoki, Eleonora Troja, Sarah V. White, Hibiki Yama
Figure caption: PRIME all-sky grid fields in equatorial coordinates. The purple and blue lines indicate the Galactic equator and b = ±30°, respectively. Red dots show the fields observed as of 2025 May 7, covering 40.8% of the sky accessible to PRIME (shaded in gray).
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Demonstrating the errors in Δmag0 that arise when the coupling between the planet signal and the noise factors is not accounted for. The observing scenario used for this plot is 1 day of integration time, the “OPTI_NF_Imager” observing mode from the Roman CGI ETC, the target planet is fixed to an angular separation of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2955, the zodiacal light surface brightness is fixed to ﹩23\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩, and the exozodiacal light surface brightness is fixed to ﹩22\ {\rm{mag}}\ {{\rm{arcsec}}}^{-2}﹩. The target stars shown are the defaults in the Roman CGI ETC.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: The results of observing each ground truth planet at its maximum ﹩{P}_{{\rm{\det }}}(t,{t}_{{\rm{int}}})-\lambda {t}_{{\rm{int}}}﹩ value when λ = 0.01 and tint is expressed in days. The “Selected ﹩{P}_{{\rm{\det }}}﹩” value is the ﹩{P}_{{\rm{\det }}}﹩ value at the maximum ﹩{P}_{{\rm{\det }}}(t,{t}_{{\rm{int}}})-\lambda {t}_{{\rm{int}}}﹩ value. We see that the summed probability of detection, ﹩{\rm{\Sigma }}{P}_{{\rm{\det }}}﹩, closely matches the number of detections, ﹩{N}_{{\rm{\det }}}﹩, that are made when the observations are simulated with the ground truth planets at the t and tint values at the selected ﹩{P}_{{\rm{\det }}}﹩. The true κEZ value for all systems is five, meaning the left plot underestimates the level of exozodi (κEZ = 1) when calculating ﹩{P}_{{\rm{\det }}}﹩, the middle plot uses the exact exozodi (κEZ = 5), and the right plot overestimates the exozodi (κEZ = 10). The color of the circles represents the true planet’s geometric albedo. Generally, planets that are not detected have low geometric albedos.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: 12″ × 12″ cutouts of the four most CO-luminous SQuIGG﹩\overrightarrow{L}﹩E  galaxies in the new sample. For each galaxy, we show the HSC i-band image, the 2 mm continuum image (collapsing the three ALMA spectral windows that were not centered on CO(2–1)), the CO(2–1) Moment 0 image, the CO(2–1) Moment 1 image, and the collapsed CO(2–1) spectrum within a 2″ aperture (also indicated as a red circle). In all ALMA images, the synthesized beam is shown as a gray circle, and contours of 2σ, 4σ, 6σ, and 8σ are shown as increasingly thick lines. The velocity region integrated to measure the CO flux is shown with dashed lines.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: RV orbit fit of a simulated habitable zone planet on a nearly edge-on orbit from simulated EPRV data. Fit was done using RVSearch (L. J. Rosenthal et al. 2021). The top row (a) overlays the observed RV data on the fitted planet’s RV signal. The middle row (b) shows the residual RV signal when the fitted planet’s RV signal is subtracted. The bottom row (c) shows the fitted planet’s signal over a single period and the observed RV data phase folded into a single period. The bottom row additionally marks the planet’s fitted period P, eccentricity e, and RV semiamplitude K. This orbital fit closely matches the “true” planet’s orbital parameters of P = 370.03 days, K = 0.031 m s−1, and e = 0.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Results of a simulation similar to Figure 14 but selecting the observation with the maximum ﹩{P}_{{\rm{\det }}}(t,{t}_{{\rm{int}}})/{t}_{{\rm{int}}}﹩ value for each planet. This selection criterion results in selecting much lower tint and ﹩{P}_{{\rm{\det }}}﹩ values. However, we see that the scenarios where the assumed ﹩{N}_{{\rm{\det }}}﹩ is not underestimated, the middle and right plots, the ﹩{N}_{{\rm{\det }}}﹩ is significantly higher than ﹩{\rm{\Sigma }}{P}_{{\rm{\det }}}﹩. Overall the observations from this method result in more efficient use of observing time.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: SQuIGG﹩\overrightarrow{L}﹩E  is an SDSS-selected sample of 1318 massive (﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\sim 11.2﹩) post-starburst galaxies at z ∼ 0.7 (gray contours; K. A. Suess et al. 2022a). Previous observational work observing CO(2–1) in these galaxies preferentially targeted the brightest (highest-mass/lowest-z) galaxies (blue points; K. A. Suess et al. 2017; R. Bezanson et al. 2022). In this work, we quadruple our sample size and target a much more representative sample (black points).
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Propagation of the fitted orbits from Figure 11 compared to the propagation of the true planet. Each subplot is titled with the length of time passed since the final RV observation was made. The true planet remains within the set of fitted orbits, which shows the fitted orbits are accurately describing the planet’s α and Δmag values. Because the fit has errors on the orbital parameters there is some dispersion among the fitted orbits. The true planet often appears near the small separation edge of the density function due to the nearly edge-on orbit (﹩i=76\mathop{.}\limits^{^\circ }25﹩). In this case the true planet was simulated with a geometric albedo of 0.16.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Probability of detection values for the Earth-like exoplanet and orbit fit shown in Figure 11 using a 6 m telescope similar to the projected HWO from R. Morgan et al. (2022). The different columns represent different assumed exozodi values with the left plot underestimating the true exozodi, the middle plot having the exact exozodi of the planetary system, and the right overestimating the exozodi. The white line represents the true detectability of the planet, any observation made at an integration time greater than the white line’s value will result in a successful detection. The figure shows that the probability of detection closely tracks the true planet’s detectability. Both the probability of detection and true detectability are calculated for a single-visit detection with an SNR threshold of seven.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Fit of the two-component exozodiacal light model (Equation C2) to the local zodiacal light data from C. Leinert et al. (1998) Table 19. The model separates the contributions from reflected sunlight and thermal emission from dust at 261.5 K. The derived scaling factors fstar and fthermal are used to model the exozodi spectra of other stars.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Demonstration of the new SED fitting adopted in this work, including MIR and FIR photometry along with AGN and galaxy dust templates. Here, we highlight J1157+0132, a galaxy that is detected in the MIR, in ancillary Herschel/SPIRE 250  μm imaging, and is the most luminous in CO in our sample. In the top left, we show the SDSS spectrum (smoothed with a 5 pixel boxcar), along with the best-fitting models for both the τBC Tied (pink) and τBC Free (gray) fits, which are virtually indistinguishable except for in [O III] emission (which is masked in the fit). In the top right, we show the posteriors for the instantaneous (t < 10 Myr) SFRs for these two fits. In the middle row, we show the best-fitting star formation history (with 1σ uncertainties) in the age period probed by our flexible bins, omitting the poorly constrained early Universe fixed-bin star formation. We also show five individual draws from the posterior to illustrate the actual resolution of the fitting. In the bottom row, we show the best-fitting SEDs, with individual components for the contributions of the AGN torus (light blue), star formation (t < 10 Myr old stellar populations and the dust heated by them), and older stars (t > 10 Myr stellar populations and the dust heated by them). We show the intrinsic stellar population (before dust attenuation) in magenta. We also show the residuals (data–model) of the photometric fit, with the shaded region indicating ±2. In the τBC Tied fit, essentially the entire IR SED is produced by the evolved, post-starburst population, but it is deficient by a factor of ∼2 relative to the 250  μm photometry. However, in the τBC Free fit, dust-obscurved star formation contributes a very similar fraction of the total IR luminosity to older stars, and the fit is better able to reproduce the observed Herschel photometry due to a small (∼0.15 dex) boost to the total IR luminosity.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption:  ﹩{M}_{{{\rm{H}}}_{2}}﹩ mass (assuming r21 and αCO = 4.0, left) and molecular gas fraction (right) vs. post-starburst time (defined as the time at which the galaxy formed 99% of the total mass formed in the Gyr before observation, as measured from the τBC Free fits). We show SQuIGG﹩\overrightarrow{L}﹩E  points in black, with CO-detected galaxies as large symbols and CO upper limits as smaller symbols. A stack of all nondetections is shown as a red square at the median tPSB. Similar to the trend with the time since quenching reported in R. Bezanson et al. (2022), we find that only the youngest SQuIGG﹩\overrightarrow{L}﹩E  galaxies are CO-luminous. In purple, we show a best-fitting exponential to the gas fraction as a function of age with a decay timescale of 70  ±  20 Myr, implying that galaxies must clear out their remaining molecular gas reservoirs in ≲150 Myr to match the observed trend.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Redshift vs. molecular gas fraction for passive galaxies with ﹩\mathrm{log}({M}_{\odot }/{M}_{\star })\gt 10.8﹩. We show the scaling relation for star-forming galaxies with ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })=11﹩ from L. J. Tacconi et al. (2018) in blue with the shaded region denoting 0.3 dex scatter. Low- (T. A. Davis et al. 2016) and high-z (M. T. Sargent et al. 2015; R. Gobat et al. 2018; J. Spilker et al. 2018; J. N. Caliendo et al. 2021; G. E. Magdis et al. 2021; K. E. Whitaker et al. 2021b; C. C. Williams et al. 2021; S. Adscheid et al. 2025) quiescent galaxies are shown as red circles and squares, respectively, with white outlines indicating measurements from individual sources and black outlines indicating measurements from stacking. Similarly, low- and high-z post-starburst galaxies from the literature are shown as green circles (K. D. French et al. 2015; K. Alatalo et al. 2016b; D. Baron et al. 2023) and diamonds (J. Spilker et al. 2018; P.-F. Wu et al. 2023; A. Zanella et al. 2023; K. A. Suess et al. 2025). When literature measurements are of dust continuum, δGDR = 100 is adopted; these measurements are indicated with × behind their point. Finally, as black circles, we show the SQuIGG﹩\overrightarrow{L}﹩E  sample. In contrast with older quiescent galaxies, which tend to have very low molecular gas fraction across cosmic time, post-starburst galaxies exhibit a wide spread in the molecular gas fraction. This is exemplified by SQuIGG﹩\overrightarrow{L}﹩E, where some galaxies have gas fractions high enough to place them on the main sequence, and some galaxies have fractions that are constrained to lie more than an order of magnitude below.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Demonstration of the new SED fitting adopted in this work, as in Figure 6. Here, we highlight J1141-0109, a galaxy that is not detected in the MIR, ancillary Herschel imaging, or in CO(2–1). While it is not included in the fit, we also indicate the characteristic 3σ uncertainty on a Herschel/SPIRE 250 μm point source based on nearby objects in the point source catalog. In contrast with the IR-detected galaxies, galaxies that are not IR-luminous return very similar star formation histories for both fits, regardless of the value of τBC, because the MIR nondetections place a ceiling on the amount of star formation that can occur behind optically thick dust.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Star-forming main sequence, with the best fit from J. Leja et al. (2022) at z = 0.7 shown (with 0.3 dex scatter in blue) and the K. E. Whitaker et al. (2012b) fit shown in purple. On the left, we show the measurements from our τBC Tied fits (pink), and on the right, we show our τBC Free fits. For clarity, for all SFRs where the median is below 0.1 M⊙ yr−1, we show the 3σ upper limit. Maximal buried star formation can raise the SFRs of SQuIGG﹩\overrightarrow{L}﹩E  galaxies, with a median offset of 0.5 dex in sources with SFRBuriedSFAllowed > 1 M⊙ yr−1, to place them at most on the J. Leja et al. (2022) main sequence (but still essentially allow below the K. E. Whitaker et al. 2012b main sequence). However, there is considerable uncertainty in those dust-obscured SFRs, and in every model, the posterior for the SFR in the τBC Free fit overlaps significantly with the posterior of the τBC Tied fit.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Demonstration of the new SED fitting adopted in this work, as in Figure 6. Here, we highlight J0910+0218, our second most CO-luminous galaxy that is detected in the MIR and in ancillary Herschel imaging. In contrast with J1157+0132 (see Figure 6), both the τBC Tied and τBC Free fits can provide a good match to the full SED, including Herschel. Even in the case where higher τBC allows for a somewhat higher SFR, the total IR luminosity is essentially identical between these models.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Comparison of the inferred total IR luminosity (defined as the total luminosity coming from all dust components in our modeling) between the two sets of models. We label the median logarithmic offset and scatter in the offset (τBC Free - τBC Tied). The two fits recover extremely similar total IR luminosity, which is well constrained by the combination of WISE and 2 mm data under the assumption of the B. T. Draine et al. (2007) galaxy dust templates and the CLUMPY torus templates (M. Nenkova et al. 2008). Any increase in the fractional contribution to the IR luminosity from buried star formation must be compensated for by a decrease in the fractional contribution from older stars, the MIR AGN luminosity, or changes to the dust temperature distribution or PAH mass fraction.