adsabs/AstroCLIMB huggingface dataset:
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Top: A comparison of the gri light curves for SN 2025ulz (black), SN 2016gkg (blue; L. Tartaglia et al. 2017), SN 2022hnt (orange; J. R. Farah et al. 2025a), and AT 2017gfo (red; V. A. Villar et al. 2017). For SN 2025ulz, we choose an explosion date of MJD=60904 based on our shock-cooling modeling (see Section 4.2). The best-fit (i.e., lowest sum of the residual squared) r-band KN model (from D. Kasen et al. 2017) to SN 2025ulz for the early-time (δt ≤ 6 days) light-curve decline is shown as a solid line. We also show the r- (black dashed line) and g-band (black dotted line) models for SN 2016gkg from A. L. Piro et al. (2017). At phase δt ≲ 6 days all four observed light curves appear to redden as they fade rapidly at around the same rate. At δt ≳ 6 days, the light curves of SN 2025ulz and the other SNe IIb begin to rebrighten while the KN light curve continues to fade rapidly. Bottom: The g − r color evolution of SN 2025ulz as compared to AT 2017gfo, SN 2016gkg, SN 2022hnt, and seven other SNe IIb (SN 1993J, M. W. Richmond et al. 1994; SN 2008ax, A. Pastorello et al. 2008; SN 2011dh, I. Arcavi et al. 2011; SN 2011ei, D. Milisavljevic et al. 2013; SN 2011fu, A. Morales-Garoffolo et al. 2015; SN 2013df, A. Morales-Garoffolo et al. 2014; SN 2024uwq, B. M. Subrayan et al. 2025). The color evolution of SN 2025ulz is very similar to the rest of the SNe IIb population.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Comparison of the MMT optical spectrum of SN 2025ulz (black) to the type IIb SN 2022hnt (orange; J. R. Farah et al. 2025a), SN 2016gkg (sky blue; L. Tartaglia et al. 2017), and the KN AT 2017gfo (red; E. Pian et al. 2017), all at similar phases. The low opacity colored regions behind the spectra show the 1σ uncertainty and the gray vertical strips are regions of telluric features. The spectral features from SN 2025ulz appear most similar to SN 2022hnt and do not show any similarity with AT 2017gfo. Most notably, the broad P-Cygni Hα feature highlighted in dark blue, present in both SN 2025ulz and SN 2022hnt, is not expected, nor seen, in the KN spectrum.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: The shock-cooling model envelope mass versus progenitor radius for SN 2025ulz as compared to a population of SNe IIb. SN 2025ulz lies in a similar region of parameter space to the other SNe IIb and is in nearly the same region as SN 2016gkg using the same model. SNe highlighted in bold have values derived from similar shock-cooling modeling, while the others adopt values from alternate methods. Points with the right half-filled are from the N. Sapir & E. Waxman (2017) BSG model and points with the left half-filled are from the N. Sapir & E. Waxman (2017) RSG model. Published values for other SNe in this figure are obtained from: SN 1993J: S. E. Woosley et al. (1994), SN 2008ax: A. Pastorello et al. (2008), R. A. Chevalier & A. M. Soderberg (2010), SN 2011dh M. C. Bersten et al. (2012), SN 2011ei: D. Milisavljevic et al. (2013), SN 2011fu: A. Morales-Garoffolo et al. (2015), SN 2013df: A. Morales-Garoffolo et al. (2014), SN 2016gkg: I. Arcavi et al. (2017a), SN 2017jgh: P. Armstrong et al. (2021), SN 2020bio: C. Pellegrino et al. (2023), SN 2022hnt: J. R. Farah et al. (2025b), SN 2024uwq: B. M. Subrayan et al. (2025), SN 2024abfo: A. Reguitti et al. (2025), and K. K. Das et al. (2023).
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: The radio light curves of SN 2025ulz (downward triangles as limits) as compared to SN 2016gkg (squares; N. A. J. et al. 2022), a sample of short SGRB radio detections (diamonds; E. Berger et al. 2005; A. M. Soderberg et al. 2006; A. J. Levan et al. 2009, 2024; W. Fong et al. 2014, 2015, 2021, 2025; A. J. Nayana & P. Chandra 2014; G. P. Lamb et al. 2019; W.-f. Fong et al. 2022; T. Laskar et al. 2022; L. Rhodes et al. 2023; G. E. Anderson et al. 2024; A. E. Nugent et al. 2024; G. Schroeder et al. 2024, 2025a, 2025b, 2025c; J. An et al. 2025b; D. Dimple et al. 2025; R. Ricci et al. 2025a, 2025c), and AT 2017gfo (plus signs; K. D. Alexander et al. 2017, 2018; G. Hallinan et al. 2017; S. Kim et al. 2017; D. Dobie et al. 2018; R. Margutti et al. 2018; K. P. Mooley et al. 2018a, 2018b, 2018c; L. Resmi et al. 2018; G. Ghirlanda et al. 2019; A. Hajela et al. 2019; E. Troja et al. 2019; J. W. Broderick et al. 2020; S. Makhathini et al. 2021). The color of the point is the representative frequency of the receiver used for the observation. Our radio limits on SN 2025ulz rule out an SGRB-like on-axis jet but do not rule out SN IIb-like or late-rising AT 2017gfo-like radio emission.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Fits of the griI and HST F336W (which is comparable to Swift/UVOT U band) light curves of SN 2025ulz with a shock-cooling modeling (N. Sapir & E. Waxman 2017), assuming two polytropic indices: n = 3/2 (left) and n = 3 (right). The best-fit explosion date, with uncertainties, and the detection date of S250818k are shown as gray and purple dashed lines, respectively.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: The International Gravitational Wave Network skymap credibility contours (orange: 50%, white: 90%) of S250818k, and the locations of all 121 candidates we found within the 95% credibility region from the Transient Name Server. The color of the point represents the overall score from our vetting, which is described in Section 5.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: A false color image of the HST WFC3 observations of SN 2025ulz. We include the F606W image from August 26 (blue; δt ∼ 8 days), the F110W image from August 27 (green; δt ∼ 9 days), and the F160W image from 2025 August 28 (red; δt ∼ 10 days). We highlight the position of SN 2025ulz showing its close in projection to the core of its host galaxy.
Paper: Optimizing Kilonova Searches: A Case Study of the Type IIb SN 2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k
Authors: Noah Franz, Bhagya Subrayan, Charles D. Kilpatrick, Griffin Hosseinzadeh, David J. Sand, Kate D. Alexander, Wen-fai Fong, Collin T. Christy, Jeniveve Pearson, Tanmoy Laskar, Brian Hsu, Jillian Rastinejad, Michael J. Lundquist, Edo Berger, K. Azalee Bostroem, Clecio R. Bom, Phelipe Darc, Mark Gurwell, Shelbi Hostler Schimpf, Garrett K. Keating, Phillip Noel, Conor Ransome, Ramprasad Rao, Luidhy Santana-Silva, A. Souza Santos, Manisha Shrestha, Ramya Anche, Jennifer E. Andrews, Sanchayeeta Borthakur, Nathaniel R. Butler, Deanne L. Coppejans, Philip N Daly, Kathryne J. Daniel, Paul C. Duffell, Tarraneh Eftekhari, Carl E. Fields, Alexander T. Gagliano, Walter W. Golay, Aldana Grichener, Erika T. Hamden, Daichi Hiramatsu, Harsh Kumar, Vikram Manikantan, Raffaella Margutti, Vasileios Paschalidis, Kerry Paterson, Daniel E. Reichart, Mathieu Renzo, Kali Salmas, Genevieve Schroeder, Nathan Smith, Kristine Spekkens, Jay Strader, David E. Trilling, Nicholas Vieira, Benjamin Weiner, Peter K. G. Williams
Figure caption: Model of our Keck spectrum that is dominated by emission from the SN 2025ulz host. We use this model to derive an SFR for the host galaxy for comparison with our radio derived SFR.
Paper: Dust Recycling and Icy Volatile Enhancement (DRIVE): A Novel Method of Volatile Enrichment in Cold Giant Planets
Authors: Eric R. Van Clepper, Felipe Alarcón, Edwin Bergin, Fred J. Ciesla
Figure caption: (a) Schematic diagram illustrating the vertical stirring of dust and expected CO enrichment. Initially, the vertical column has a uniform dust-to-gas mass ratio, ε, shown in black, and gas phase CO abundance, XCO = XCO,0, shown in red, above the sublimation height, Zsub (top). Typically, dust growth and settling concentrated dust mass near the midplane, with CO gas depleted as a result of the cold finger effect (middle). In the DRIVE mechanism, dust is puffed vertically from planetary stirring carrying CO ice above the sublimation height. CO ice is then sublimated into the gas phase, with the abundance of CO proportional to the integrated dust-to-gas mass ratio above Zsub, indicated by the hatched region. (b) Expected CO abundance relative to the initial abundance, fCO, as a function of Zsub and fα. fCO is calculated from the DustPy simulation after 1 Myr of evolution in the pressure bump for fragmentation velocities of 1 m s−1 (left) and 10 m s−1 (right). The CO sublimation surface where dust temperatures reach 30 K is shown by the red dashed line, while the gas scale height is shown by the gray dotted line. The dust scale height is increased using a diffusivity of fαα, accounting for vertical stirring as a result of meridional flows. We find that for Zsub/R < 0.1, dust densities (and thus CO abundances) are near or above expected solar metallicities in all cases.
Paper: Dust Recycling and Icy Volatile Enhancement (DRIVE): A Novel Method of Volatile Enrichment in Cold Giant Planets
Authors: Eric R. Van Clepper, Felipe Alarcón, Edwin Bergin, Fred J. Ciesla
Figure caption: Dust distribution as a function of size and radius from DustPy simulations showing the initial conditions of the dust size distribution (top row) and after 1 Myr of evolution (center row) for a disk containing a Jupiter-mass planet located at 75 au. We examine disks with particle fragmentation velocities of 1 m s−1 (left column) and 10 m s−1 (right column). The grain size distribution in the pressure bump at 101 au is shown in the bottom row. Regardless of dust fragmentation velocity, we see an enhancement of small dust less than St = 10−3 (dotted line) in the pressure bump. The total dust-to-gas mass ratio, ε, is labeled in each plot, where the initial dust-to-gas is ε = 0.01 in the outer disk. The dust-to-gas mass ratios for grains with St ≤ 10−3, εsm, and St > 10−3, εlg, are also shown. For the case with larger fragmentation velocity, while the total dust mass is higher and the grains reach much larger sizes, the total mass of dust with St​​​​​​ ≤ 10−3 is about 0.01 in both cases.
Paper: Dust Recycling and Icy Volatile Enhancement (DRIVE): A Novel Method of Volatile Enrichment in Cold Giant Planets
Authors: Eric R. Van Clepper, Felipe Alarcón, Edwin Bergin, Fred J. Ciesla
Figure caption: Cartoon schematic of the DRIVE effect enriching the atmosphere of a giant planet with volatiles. Larger pebbles trap volatiles from the outer disk and transport them to the pressure bump created by the giant planet via radial drift. Here, fragmentation creates fine dust, which can be lofted away from the midplane, leading to sublimation of ice mantles on the dust and enriching the gas above the snow surface with volatiles. This volatile-rich gas can then be accreted onto the planet, resulting in a volatile-enriched atmosphere. The dust, due to the lower gas density at the surface of the disk, decouples from the gas and can settle back to the midplane as a bare grain, fractionating the volatile elements from the more refractory solids. Here, the color shows the azimuthally averaged gas density from our FARGO3D simulations. The solid black contour outlines the region of the disk where the total dust-to-gas mass ratio is equal to 0.01 in our DustPy simulations, with higher dust densities below this contour. The transport of icy pebbles is represented by the black and red solid arrows, where black arrows represent bare grains and red arrows represent CO gas. Meridional flows onto the planet including entrained CO gas are illustrated by the red and black dashed arrows. The approximate location of the CO snowline at 30 K is also included.
Paper: Dust Recycling and Icy Volatile Enhancement (DRIVE): A Novel Method of Volatile Enrichment in Cold Giant Planets
Authors: Eric R. Van Clepper, Felipe Alarcón, Edwin Bergin, Fred J. Ciesla
Figure caption: Azimuthally averaged gas density (left) and gas radial velocity relative to the planet (right) for our FARGO3D disk model containing a Jupiter-mass planet at 75 au. The CO sublimation surface at 30 K recovered from our RADMC-3D model is indicated in both panels by the red dashed line. The region near the embedded planet is heated from a combination of accretion heating onto the planet, disk viscous heating, and radiative heating from the star, resulting in higher temperatures at the midplane in the gap. Gas advection relative to the local sound speed is also indicated by white arrows. Gas advection is primarily outward along the midplane near the planet, with significant vertical flows away from the midplane at the gap edge and in the pressure bump at 100 au.
Paper: Dust Recycling and Icy Volatile Enhancement (DRIVE): A Novel Method of Volatile Enrichment in Cold Giant Planets
Authors: Eric R. Van Clepper, Felipe Alarcón, Edwin Bergin, Fred J. Ciesla
Figure caption: (Top) Particle trajectory of the tracer particle reaching the maximum temperature, with the hottest point labeled with a red dot. The background color and arrows show the azimuthally averaged gas density and advection. This particle is lofted to high altitude following the meridional gas circulation in the disk, reaching temperatures up to 55 K. The particle’s temperature along its trajectory is shown by the color of the line. The particle temperature is shown over 20 kyr to demonstrate the particle’s trajectory before and after reaching the hottest point at 0.3 Myr. This particle’s height above the midplane (middle) and temperature (bottom) are also shown as a function of time over the full 1 Myr integrated by the red lines. Examples of other particles are also shown in black, indicating that the highlighted particle’s trajectory and temperature are typical of other similarly sized particles.
Paper: Dust Recycling and Icy Volatile Enhancement (DRIVE): A Novel Method of Volatile Enrichment in Cold Giant Planets
Authors: Eric R. Van Clepper, Felipe Alarcón, Edwin Bergin, Fred J. Ciesla
Figure caption: The maximum temperature reached by particles of different sizes, ranging from 1 mm to 1 μm (right column) for particles starting at the midplane at 100 au. The color map shows the number of particles out of 1000 total that have reached a given temperature as a function of time. Also indicated in each plot by a solid line is the 50th percentile for the maximum temperature reached as a function of time. The dashed lines show the 25th and 75th percentiles, and the dotted lines show the 10th and 90th percentiles. While large particles are not heated much above the midplane temperature, solids below 10 μm in size (St ≲ 10−3 ) at the midplane experience heating. All of these dust particles experience temperatures above 30 K by 1 Myr.
Paper: Colors of Life in the Clouds: Biopigments of Atmospheric Microorganisms as a New Signature to Detect Life on Planets like Earth
Authors: Lígia F. Coelho, Lisa Kaltenegger, William Philpot, Adam J. Ellington, Noelle Bryan, Stephen Zinder, Brent C. Christner
Figure caption: Relative reflectance spectra of seven aerial microorganisms of wet (top panel) and dry (middle panel) measurements, and absolute reflectance (bottom panel—dashed lines for dry biota; solid lines for wet biota) with zoomed-in visible range wavelength panel on the right. Control (black lines in the bottom panel) refers to a filter with culture medium only, where wet control refers to fresh medium and dry control refers to dry medium. Biopigments show features between 400 and 600 nm (see “Zoom” panels), water absorption features at 1490 nm and 1900 nm are indicated by vertical blue bands. (Data set available at doi:10.5281/zenodo.17196858).