adsabs/AstroCLIMB huggingface dataset:
Paper: Cool Dark Gas in Cygnus X: The First Large-scale Mapping of Low-frequency Carbon Recombination Lines
Authors: Kimberly L. Emig, Pedro Salas, Loren D. Anderson, D. Anish Roshi, Lars Bonne, Alberto D. Bolatto, Isabelle A. Grenier, Rebecca C. Levy, Dylan J. Linville, Matteo Luisi, M. Riley Owens, J. Poojapriyatharsheni, Nicola Schneider, Luigi Tibaldo, Alexander G. G. M. Tielens, Stefanie K. Walch, Glenn J. White
Figure caption: Red, green, and blue compilation in the Cygnus X region covering the footprint that we surveyed; in red is the CGPS 1.4 GHz continuum (A. R. Taylor et al. 2003), green is MSX 8 μm PAH emission (N. Schneider et al. 2006), and blue is 13CO (1–0) tracing (some of the) molecular gas (N. Schneider et al. 2010). Left: the numbers enclosed by a circle in black indicate the “DR” continuum sources identified in 5 GHz observations by D. Downes & R. Rinehart (1966), which are mostly thermal H II regions, except for DR3 and DR4, which make up the SNR γ Cygni. Dotted circles show the Cyg OB2 association and open clusters NGC 6910 and NGC 6913. The region at ℓ > 80° commonly referred to as Cyg X North and at ℓ < 80° (also typically at lower latitudes) referred to as Cyg X South are also indicated. Right: contours of velocity-integrated C273α (moment 0), drawn at [3, 5.5, 8, ...28]σ. C273α is detected from 75% of the mapped region.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: Posterior probability distributions from Prospector fitting of NIRSpec, NIRCam, and MIRI data. From left to right, the columns show the posterior distributions for redshift (z), stellar mass (M*), gas-phase metallicity (Zgas), star formation rate in the past 10 Myr (SFR10), dust attenuation in the V band (AV) for young stars, the column density of neutral hydrogen (NHI), the IGM factor (fIGM), the escape fraction of ionizing photons (fesc), and the ionization parameter (U). The diagonal panels display the 1D marginalized posterior distributions for each parameter, with dashed lines indicating the 16th, 50th, and 84th percentiles. The upper right panel shows the inferred star formation history as a red step plot, with the red shaded region indicating the 16th–84th percentile range of the posterior distribution, and the gray shaded region showing the same percentile range for the prior. The lower x-axis indicates look-back time from the inferred redshift of JADES-GS-z14-1 (z = 13.86), while the upper x-axis shows the corresponding redshift. The y-axis represents the star formation rate.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: Surface brightness profile of JADES-GS-z14-1 in the NIRCam F182M, F200W, and F210M bands, compared with the model PSF in the mosaic images (mPSF), Sérsic models with effective radii re = 15 mas and 30 mas, and a brown dwarf. The mPSF is constructed with STPSF using the spectrum of JADES-GS-z14-1. Sérsic models are generated using the GALFIT package assuming a Sérsic index n = 1 and zero ellipticity, and are convolved with the mPSF. χ2 values are computed by fitting the fluxes while keeping the profiles fixed within 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 cutouts. The brown dwarf is not spatially resolved and has brightness comparable to JADES-GS-z14-1 in these bands.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: Posterior distribution of the [O III]/Hβ flux ratio and the equivalent width EW([O III] + Hβ), derived from Prospector fits to MIRI/F770W, NIRCam, and NIRSpec data for JADES-GS-z14-1. The color scale transitioning from red to white indicates the posterior density, with black contours marking the 1σ, 2σ, and 3σ levels. The black-edged diamond with gray error bars marks JADES-GS-z14-0 from MIRI photometry (J. M. Helton et al. 2025). The gray shaded region indicates the 16th–84th percentile range of EW([O III] + Hβ) from a photometric z ≈ 7 sample, with the dashed line showing the median (R. Endsley et al. 2023). Colored points represent JADES DR3 galaxies at z ≳ 7 from NIRSpec observations, with color indicating the absolute UV magnitude MUV; triangles denote 3σ lower limits for galaxies without Hβ detections (F. D’Eugenio et al. 2025). The [O III] lines refer to the [O III] λλ4959, 5007 doublets.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: (a) False-color image of JADES-GS-z14-1, showing the relative positions of MIRI and NIRCam emission. The white circle marks a MIRI/F770W hotspot near the target, where the circle has a diameter equal to the FWHM of the MIRI/F770W PSF. (b) JWST MIRI/F770W mosaic image, with blue concentric circles indicating the annuli used for extraction of the surface brightness profile of JADES-GS-z14-1. Gray hatched regions mark areas with significant contamination by a foreground galaxy. Both the hotspot and the hatched regions are masked during the measurement of the surface brightness profile of JADES-GS-z14-1. (c) Surface brightness profile of JADES-GS-z14-1 in the MIRI/F770W band in comparison with the MIRI/F770W empirical PSF (ePSF) and the profiles of JADES-GS-z14-0 and the hotspot. The profiles are normalized by the flux in the first aperture. All images are oriented with north up and east to the left.
Paper: JADES-GS-z14-1: A Compact, Faint Galaxy at z ≈ 14 with Weak Metal Lines from Extremely Deep JWST MIRI, NIRCam, and NIRSpec Observations
Authors: Zihao Wu, Daniel J. Eisenstein, Benjamin D. Johnson, Peter Jakobsen, Stacey Alberts, Santiago Arribas, William M. Baker, Andrew J. Bunker, Stefano Carniani, Stéphane Charlot, Jacopo Chevallard, Mirko Curti, Emma Curtis-Lake, Francesco D'Eugenio, Kevin Hainline, Jakob M. Helton, Tiger Yu-Yang Hsiao, Xihan Ji, Zhiyuan Ji, Tobias J. Looser, George Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Fengwu Sun, Sandro Tacchella, James A. A. Trussler, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok, Yongda Zhu
Figure caption: SED modeling of JADES-GS-z14-1 using the Prospector package. (a) Observed NIRCam and MIRI/F770W photometry is shown as green filled circles with 1σ error bars. The coadded NIRSpec spectrum is displayed as a blue step plot, with shaded regions indicating the 1σ uncertainties. The orange curve represents the best-fit spectral flux density, and the shaded orange region denotes the 16th–84th percentile range of the posterior. Orange squares indicate the synthetic photometry corresponding to the best-fit model. (b) Residuals expressed as χ values, defined as the difference between the observed data and the best-fit model, normalized by the measurement uncertainties. (c) Transmission curves for the relevant filters, with filter names labeled at right. For the NIRCam long-wavelength channel, the photometry and transmission curves for Models A and B are shown separately. The F277WA band is identified as an outlier and is therefore excluded from the modeling and not shown in the plot.
Paper: Massive Double White Dwarf Binary Mergers from the Moon: Extending the Reach of Multimessenger Astrophysics
Authors: Manuel Pichardo Marcano, Anjali B. Yelikar, Karan Jani
Figure caption: Evolution of the characteristic strain as a function of gravitational-wave frequency over 1 yr before merger for all massive (individual masses M > 1M ⊙ ) WD mass combinations at a distance of 10 Mpc. The color gradient represents the lower component mass for each double WD binary considered. We consider two distinct merger frequency definitions: the Roche lobe case in brown and the contact case in green/blue (see Section 2). The sensitivity curves of Lunar-SUS, LISA, and Lunar-SEI are overlaid in purple, red, and orange, respectively.
Paper: Massive Double White Dwarf Binary Mergers from the Moon: Extending the Reach of Multimessenger Astrophysics
Authors: Manuel Pichardo Marcano, Anjali B. Yelikar, Karan Jani
Figure caption: One year sky-averaged detection distance for three different WD mass combinations. For the average detection distance calculation, we integrate Equation (5) over a 1 yr period, setting ﹩{f}_{{\rm{\min }}}﹩ as the frequency 1 yr before merger and ﹩{f}_{{\rm{\max }}}﹩ to be the merger frequency. We consider both the contact and Roche lobe cases (see Section 2), respectively. We reiterate that the contact case is not physically realistic, as WDs would undergo significant tidal disruption before merger and should be seen as an idealized upper limit for detection distance. Results are shown for both Lunar-SUS and Lunar-SEI detectors, comparing the contact case (solid bars) and Roche lobe overflow case (hatched bars) scenarios. LISA’s detection range (orange) remains nearly constant at ∼0.4 Mpc across all mass combinations.
Paper: Massive Double White Dwarf Binary Mergers from the Moon: Extending the Reach of Multimessenger Astrophysics
Authors: Manuel Pichardo Marcano, Anjali B. Yelikar, Karan Jani
Figure caption: Sky-averaged detection distances for all the WD mass combinations for Lunar-SUS and Lunar-SEI detectors, considering both contact (top panels) and Roche lobe (bottom panels) merger frequency definitions. The white contours indicate detection distances in Mpc, spanning from 1 to 800 Mpc as shown by the color bar to the right.
Paper: Massive Double White Dwarf Binary Mergers from the Moon: Extending the Reach of Multimessenger Astrophysics
Authors: Manuel Pichardo Marcano, Anjali B. Yelikar, Karan Jani
Figure caption: Evolution of the SNR as a function of time before merger for three representative mass combinations: 1.4 M⊙ + 1.4 M⊙(left panel), 1.33 M⊙ + 1.33 M⊙ (middle panel), and 1 M⊙ + 1.4 M⊙ (right panel), all at a reference distance of 10 Mpc. For each mass combination, we present results for both merger cases for Lunar-SUS (blue solid and orange dotted lines) and for Lunar-SEI (green dashed and red dotted lines). The horizontal black line indicates our detection threshold of ρth = 8. We
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: (Left) Resolved stars in the M82 field from ANGST (J. J. Dalcanton et al. 2009) with the stars from the Southern Arcs field (this work). The points in cyan represent populations of stars ≲400 Myr, selected by excluding the RGB stars from the CMD of each data set (dashed gray regions in the panels on the right) with matched depths (F814W < 26). The M82 disk has been masked out for these stars to accentuate structures that follow the breakout of the outflow from the disk. Arc-like features in the Southern Arcs field appear to be spatial extensions of young stellar structures in ANGST that may be related to M82’s starburst outflow. (Top Right) F814W vs. F435W-F814 CMD of GST sources from ANGST with some typical PARSEC (A. Bressan et al. 2012) isochrones (shifted assuming AV = 0.1 and (m − M)0 = 27.8). The 10 Gyr isochrones have metallicities, [M/H] = 0, −0.5, −1.0, −1.5, −2.0. The younger isochrones have [M/H] = 0. (Bottom Right) CMD of “GST” sources from the Southern Arcs. PARSEC isochrones with a foreground extinction (shifted assuming AV = 0.35 and (m − M)0 = 27.8) are overplotted to broadly explain the multiple stellar populations. The 10 Gyr isochrones ([M/H] = 0, −0.5, −1.0, −1.5, −2.0) correspond to the old, RGB halo stars. The 100 Myr isochrone accounts for some of the fainter main-sequence stars and most of horizontal branch core helium burners (HeB). The 30 Myr isochrone accounts for the brighter main-sequence stars, HeBs, and red supergiants. We assume an [M/H] = −0.25 for the ≤500 Myr isochrones.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: HST’s WFC3 footprint of this work overlaid on the gri color image of M82 from Subaru Hyper Suprime Cam (A. Smercina et al. 2020).
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: Completeness of photometry in the Southern Arcs as a function of input magnitude (left) and photometric bias or error in recovered magnitudes as a function of input magnitude for the F475W (top right) and F814W (bottom right) filters from ASTs.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: Multiwavelength overview of M82’s outflow and its resolved stellar populations. (Left) The colormap represents the far-UV intensity from GALEX (GII-36; PI: John Huchra). Most of the observed far-UV photons originate from the continuum emission of the starburst regions, scattered into our line of sight by dust in the outflow. Faint far-UV emission is also detected along the young stars in the Southern Arcs. H I contours (W. J. G. de Blok et al. 2018), tracing neutral hydrogen at levels of 0.3, 0.6, and 1.2 Jy/beam km s−1, are shown as solid white lines. Spitzer-IRAC4 contours, which trace hot dust emission at 8 μm (SINGS1_159; PI: Robert Kennicut) at levels of 1, 4, and 16 au (arbitrary units), are shown as dashed yellow lines. (Right) Archival 0.35–1.1 keV (soft) X-ray image of M82 from the Chandra X-ray Observatory. Resolved young stars (≲400 Myr) from ANGST and the Southern Arcs are displayed in both panels as cyan points, with the disk of M82 masked out. In M82, soft X-ray emission originates both from the mass-loaded starburst wind itself (T ≳ 106 K) and from intermediate-temperature gas (T ∼ 106–107 K) at the shocked interfaces between the hot outflow (T ∼ 108 K) and the cooler halo medium.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: The SFH of the Southern Arcs appears correlated with the SFH of the central M82 disk. (Left) Resolved stars in the M82 field from ANGST and the Southern Arcs. Regions for which SFHs were calculated by B. F. Williams et al. (2011) (POS2 and POS5) are shown in the same plot. Locations of young massive star clusters studied by S. Li et al. (2015) are also shown for reference. (Top Right) SFHs of POS2 (cyan) and POS5 (orange) scaled down by a factor of 20 compared to the SFH of the Southern Arcs obtained from PADUA models (blue). POS2 and POS5 are dominated by stars from the central disk region of M82. The Southern Arcs and the central M82 disk both experienced enhanced star formation ∼100 Myr ago. (Bottom Right) Histogram of star cluster ages from S. Li et al. (2015) (pink) compared to the SFH of the Southern Arcs obtained from PADUA models (blue). The M82 disk experienced multiple epochs of star cluster formation similar to the Southern Arcs.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: (Left) CMD selection of ∼10 Myr and ∼100 Myr stars from model Hess diagrams generated from PADUA models. (Top Right) Spatial distribution of ∼10 Myr stars (blue) and ∼100 Myr stars (orange). (Middle Right) 2D spatial cross correlation between the ∼10 Myr and ∼100 Myr populations. Pixels that correspond to shifts along the direction of the outflow and having a correlation >0.5 are marked in green. (Bottom Right) RGB stars from the ancient halo population appear randomly distributed.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: Schematic illustration of the two mechanisms proposed for the formation of the Southern Arcs. (Left) Multiple generations of shocks from the outflow compress a cool, dense CGM cloud, triggering multiple epochs of star formation. (Right) Stars form within cool clouds associated with the outflow. The stars and clouds comove ballistically. An encounter with a second CGM cloud or tidal debris triggers a second burst of star formation in the original clouds.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: Southern Arcs: (Left) Observed Hess diagram used by MATCH that balances number statistics on the CMD with time resolution in the SFH; (Center) Best-fit model Hess diagram using PADUA stellar evolution models with complete AGB tracks (P. Marigo et al. 2008; L. Girardi et al. 2010); (Right) Residual significance Hess diagram. The color bars in the left and center panels represent the number of stars per CMD bin. In the right panel, the scaling reflects the significance of each pixel in the residual relative to the standard deviation of a Poisson distribution. The RGB mask used is shown in gray in all panels.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: Best-fit SFHs for the Southern Arcs using PADUA, MIST, and BASTI isochrones. Error envelopes represent the 68% confidence interval of random uncertainties. (Left) Absolute SFR as a function of lookback time. (Right) Cumulative fraction of stars formed as a function of lookback time. Star formation occurs in two epochs beginning at ∼150 Myr and ∼30 Myr, marked by a steepening of slopes in the cumulative SFH.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: Southern Arcs: (Left) Observed Hess diagram; (Center) Best-fit model Hess diagram using PADUA (top row), MIST (middle row), and BASTI (bottom row) stellar evolution models; (Right) Corresponding residual significance Hess diagrams.
Paper: Stars Born in the Wind: M82’s Outflow and Halo Star Formation
Authors: Vaishnav V. Rao, Adam Smercina, Eric F. Bell, Benjamin Williams, Julianne J. Dalcanton, Andrew Dolphin, Adam Leroy, Antonela Monachesi, Jeremy Bailin, Roelof S. de Jong, Fabian Walter
Figure caption: (Left) Spatial distribution of stars in the Southern Arcs field. MW foreground stars identified using Gaia DR3 (Gaia Collaboration et al. 2016, 2023) are shown with their proper motions and are circled in gray. (Right) The CMD of stars in the Southern Arcs field with a 10 Myr PARSEC isochrone overplotted. Stars with F814 < 21.5 are likely MW foreground.
Paper: The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 μm Emission in Nearby Galaxies
Authors: Edward Zhang, Andreas L. Faisst, Brendan P. Crill, Hanae Inami, Thomas Lai, Youichi Ohyama, Jeonghyun Pyo, Rachel Akeson, Matthew L. N. Ashby, James J. Bock, Yun-Ting Cheng, Yi-Kuan Chiang, Asantha Cooray, Olivier Doré, Richard M. Feder, Yongjung Kim, Bomee Lee, Daniel Masters, Gary Melnick, Roberta Paladini, Michael W. Werner
Figure caption: Top: calibration of our CIGALE models to observations from B. Gregg et al. (2024; individual star-forming regions in local galaxies) and T. S. Y. Lai et al. (2020; low-redshift star-forming galaxies). The models are shown for different qPAH (acting as a free parameter, indicated by colors) and a range of E(B − V) from 0.1 to 0.5 mag (indicated by the width of the bands). We find that a value of qPAH = 1.12% fits well the observations across more than 7 orders of magnitude in total SFRs. Bottom: comparison of our CIGALE models (red) to observed AKARI SPICY spectra (data and best fit) from Y. Ohyama et al. (2018). Stellar mass is fixed to the one measured from photometric SED fitting, and a qPAH = 1.12% is assumed. Note that the AKARI spectra cover a wavelength range redder than SPHEREx (specifically the 6.2, 7.7, 8.6, 11.3, and 12.7 μm PAH bands) and therefore miss the 3.3 μm band (indicated by the arrow). We also show photometric data from WISE (filled squares) and AKARI (open circles) for comparison.