adsabs/AstroCLIMB huggingface dataset:
Paper: Creating the Radius Gap without Mass Loss
Authors: Eve J. Lee, Amalia Karalis, Daniel P. Thorngren
Figure caption: Best-fit core mass distributions of mass-loss models compared with the radial-velocity (RV) follow-up of Kepler sub-Neptunes (RV, blue histogram) from Marcy et al. (2014). The RV distribution is not corrected for any observational biases. Wu (2019) assumes a lognormal core mass distribution and fits the photoevaporative mass-loss model to the California Kepler Survey (CKS) radius distribution from Fulton & Petigura (2018). They find a distribution that is too peaked and shifted toward too high a core mass. Gupta & Schlichting (2019) assume a Rayleigh distribution for ﹩{M}_{\mathrm{core}}\lt 5{M}_{\oplus }﹩, and ﹩{dN}/{{dlogM}}_{\mathrm{core}}\propto {M}_{\mathrm{core}}^{-1}﹩ for larger masses, and fit the core-powered envelope mass-loss model to the CKS data. Their lower-mass tail falls off too sharply. Rogers & Owen (2021) consider a nonparametric form of ﹩{dN}/{{dlogM}}_{\mathrm{core}}﹩ fitting the photoevaporative loss model to the CKS data, finding a much broader distribution. They still expect a falloff at ﹩{M}_{\mathrm{core}}\lt {M}_{\oplus }﹩.
Paper: Creating the Radius Gap without Mass Loss
Authors: Eve J. Lee, Amalia Karalis, Daniel P. Thorngren
Figure caption: Radial density profiles of a 5M ⊕ core at 0.3 au with ﹩{M}_{\mathrm{gas}}/{M}_{\mathrm{core}}=0.01﹩. The underlying disk is MMEN depleted by a factor of 100. Like Figure 4, lighter curves represent smaller R out/R Hill = (1.0, 0.55, 0.3, 0.17, 0.1) while solid and dotted lines illustrate convective and radiative zones, respectively. The small convective windows are created by a small increase in opacities at temperatures of ∼800 K, likely corresponding to the water absorption line at ∼3 μm. Smaller R out steepens the overall density profile, rendering the radiative–convective boundary more optically thick, although these differences are minimal down to R out/R Hill = 0.1.
Paper: Creating the Radius Gap without Mass Loss
Authors: Eve J. Lee, Amalia Karalis, Daniel P. Thorngren
Figure caption: Top: comparison of occurrence rate studies performed by California Kepler Survey (Fulton & Petigura 2018, <100 days; their Figure 5) and by Hsu et al. (2019, 2–64 days; their Table 2). The downward arrows denote upper limits. While the overall shape and the approximate location of the radius gap are similar between the two studies, Hsu et al. (2019) find overall broader radius distribution both toward larger radii (>3R ⊕) and smaller radii with a hint of sub-Earths (<R ⊕) becoming a dominant population. Bottom: radius distribution at different orbital periods from Hsu et al. (2019). We verify their finding that there is no evidence of decrease in small planet (≲1.4R ⊕) population at long orbital periods.
Paper: Creating the Radius Gap without Mass Loss
Authors: Eve J. Lee, Amalia Karalis, Daniel P. Thorngren
Figure caption: Envelope mass fraction of a 5 M ⊕ core at 0.3 au in MMEN, with its gas surface density reduced by a factor of 0.01. Left: how the final ﹩{M}_{\mathrm{gas}}/{M}_{\mathrm{core}}﹩ at 1 Myr scales with the outer boundary radius. We observe a weak dependence on the bound radius down to ∼0.1R out/R Hill. Right: time evolution of ﹩{M}_{\mathrm{gas}}/{M}_{\mathrm{core}}﹩ with lighter curves representing smaller R out/R Hill = (1.0, 0.55, 0.3, 0.17, 0.1), as shown on the left panel.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: An estimate for a gas distribution that may create an accumulation of millimeter-sized dust into a bright ring similar to the ALMA observation of DoAr 44. For comparison, we also plot the profile fit by van der Marel et al. (2016) to ALMA CO observations.
Paper: Creating the Radius Gap without Mass Loss
Authors: Eve J. Lee, Amalia Karalis, Daniel P. Thorngren
Figure caption: Vertical optical depth to stellar irradiation (black) and internal thermal radiation (red) vs. disk gas surface density, normalized to that of minimum mass extrasolar nebula (MMEN; Chiang & Laughlin 2013). When dust grains following the ISM grain size distribution dominate the opacity (solid lines), the disk remains optically thick at 0.1 au until the gas depletes by more than 6 orders of magnitude with respect to MMEN. When dust grains do not contribute to opacity (dashed lines), the disk becomes optically thin once the gas depletes by approximately 2 orders of magnitude.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: The evolution of the dust surface density over 105 yr using the gas distribution from Figure 17. The dust distribution from our best-fitting radiative transfer model to the ALMA data (Figure 12) is plotted as a dashed black curve. We find that dust drift alone can produce a similar distribution after ∼50,000 yr.
Paper: Dust Rings and Cavities in the Protoplanetary Disks around HD 163296 and DoAr 44
Authors: Harrison Leiendecker, Hannah Jang-Condell, Neal J. Turner, Adam D. Myers
Figure caption: Dust drift timescales (﹩r/\dot{r}﹩) for various grain sizes within the gas distribution from Figure 17. The selected size range represents the range of grain sizes that grow over time in Figure 18. Dotted lines help line up the discontinuities between sign changes in drift rates. Positive and negative values correspond to outward and inward drift, respectively. Grains smaller than 0.1 mm would not be trapped in the bright ring and may flow into the cavity.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: Example SED fitting of GOODS-S galaxies. The observed photometric data points (red circles) are fit with an SED model (cyan thick lines) composed of the FSPS stellar component (green thick lines), AGN component (blue thick lines), and SFG dust emission component (orange thick lines). The best-fit model photometry is shown as open blue squares. We also show 20 random SEDs drawn from the final MCMC chains to show the ranges of model degeneracy. Characteristics of these examples are as follows (from top to bottom and left to right): 10735—pure SFG; 5358—galaxy with a bright obscured AGN that dominates its near- to mid-IR emission; 18220—IR composite galaxy with UV–optical emission including a strong contribution from an unobscured AGN; 29988—galaxy whose UV to mid-IR emission is dominated by a moderately obscured AGN; 10260—IR composite galaxy with an obscured AGN; 20671—galaxy with a weak obscured AGN; 19765—galaxy where the existence of the AGN is highly ambiguous and we have shown the degenerate models in magenta; 24193—galaxy without enough data to detect any AGN component. The y-axis is the source flux (ν F  ν ) described in units of maggies μm–1, where 1 maggie equals 1/3631 Jy.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: 5σ flux sensitivities as a function of band wavelength for the data used in this work and sensitivities predicted for the planned JWST GTO surveys. A few AGN templates are also plotted to compare against the survey limits to demonstrate the importance of the mid-IR wavelength coverage in the identification of obscured AGNs. Two galaxy templates shifted to a redshift of 2, one for star-bursting galaxies (Arp 220) and another for quiescent galaxies (a 2 Gyr old elliptical galaxy), are shown for comparison. At a typical redshift of z ∼ 2, the 4–6 μm range provides good potential for AGN detection for both existing data and JWST MIRI-HUDF.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: The observed IR to radio flux q obs,24 as a function of redshift of all the sources. The red dotted line is 0.5 dex below the midpoint of the radio–infrared correlations in the Rieke et al. (2009) SFG templates; we define the source as a radio-loud AGN if it falls below this line at ≥2σ significance. We color-code different sources on the main plot and show their relative distribution of q obs,24 on its right side.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: Left: survey footprints of the GOODS-S: Chandra 2–7 keV (blue), 3D-HST 0.3–8.0  μm (black), Spitzer/MIPS 24 μm (red), and VLA 3 GHz (green) and 6 GHz (orange) observations. For the VLA surveys, we have denoted the sizes of the 3 and 6 GHz HPBW with dashed circles and the primary beam cutoffs with solid circles. We have also highlighted the location of radio-detected and radio-undetected AGNs in this area. Right: four small panels show the footprints of different surveys and the distributions of corresponding sources.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: Examples of the galaxy stellar (left panel), AGN (middle panel), and SFG dust emission (right panel) templates used in our SED model. We have shown the variations caused by the single parameter that leads to the most significant changes of the SED model. See the text for more details. The stellar emission is dominated by photospheric output at wavelengths <10 μm and by reradiation by circumstellar dust at longer wavelengths.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: The X-ray 0.5–7 keV intrinsic luminosity vs. the radio 3 GHz luminosity of the VLA-detected and undetected X-ray sources. The red line is the AGN identification criterion, above which the source is considered as an [xtype_x2r] AGN.
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: IRAC color–color diagram of the VLA-detected AGNs. We have denoted the selection criteria proposed by Kirkpatrick et al. (2017; magenta dashed lines) and Donley et al. (2012; yellow shaded region).
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: The standard deviations of the visibilities within a nominally redundant group of each baseline vector for the vertical (top row), horizontal (middle row), and tilting (bottom row) feed motions. The first column shows the results with the combined sky model, which is then separated into the GLEAM (second column) and GSM (third column) sky models. The color scale indicates the σ red normalized by the thermal noise of the visibility (σ th). The same value for σ th, which is 2.5 Jy, from the fiducial model, averaged over the frequency band, is used for all panels. We consider visibilities with σ feed = 3 cm for the feed translation and σ feed = 3° for the tilting. We see that diffuse emission introduces strong nonredundancy for particular baseline types, while point sources generate nonredundancy across all baselines.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: The behaviors of the main lobe of the power beam in the xz plane or in the EW direction, with different types of feed motions: x-direction (far left), y-direction (center left), z-direction (center right), and tilting feed motions in the xz plane (far right). The top row shows the line profiles of power beams that are normalized to the peaks at 165 MHz. Based on the line profiles, we measure the shift of the maximum of the main lobe (middle row) and the FWHM of the main lobe (bottom row) as a function of feed motion and frequency. When the feed moves in the x-direction or tilts in the xz plane, the main lobe shifts in the xz plane, as expected. The beamwidth changes relatively more when the feed moves in the z-direction.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: Integrated primary beams outside the main lobes of the perturbed beam, with respect to the unperturbed beam. For the translational motions shown in the first three panels, the feed displacement is labeled from −7 to 7 cm. For the tilting motion, we consider the motion in the xz plane, with the tilt measured from the zenith spanning from −6° to 6°.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: The same format as Figure 2, but for the behaviors of the primary beam in the yz plane or in the NS direction. The shift of the peak location in the main lobe is observed for the y-direction feed motion, while the change to the beamwidth mainly arises from the vertical motion or the tilting motion.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: Relative σ red of the autocorrelations for vertical (left), horizontal (middle), and tilting feed motions (right), with feed offset and frequency.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: The fiducial beam pattern (far left) and the differences of the primary beam models (B’) relative to the fiducial model (B) for feed displacement by +3 cm in the x-direction (center left), by +3 cm in the z-direction (center right), and for tilt by +3° in the xz plane (far right) at 165 MHz. The difference is normalized by the amplitude of the fiducial model. The different feed motions lead to the different beam patterns.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: The configuration of HERA-320. This highly redundant array configuration is designed to achieve high-precision calibration and deep sensitivity to the 21 cm power spectrum.
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Evolution of spin period of the J1901+1458 for ﹩\dot{M}=8.0\times {10}^{-7}{M}_{\odot }﹩ yr−1 (with B = 800 MG) and for different values of initial rotational periods, P 0 = (3.14, 108.7, 258.7, 558.7, 708.7, 814.2) s. The dotted lines divide the evolution into three stages according to the value of ω. In the first stage, the WD can start with ω > 1 or ω < 1 depending whether the initial period is below or above the equilibrium period, P eq = 388.6 s (Equation (20)), respectively. For both values, the involved torques are dipole radiation torque, T mag, and accretion torque, T acc, in the propeller phase. However, T acc is the dominant torque in this phase. For ω ≈ 1, T mag ≈ T acc and the system goes through the equilibrium period, P eq. For ω < 1, the involved torque is T dip. T acc no longer acts on the star, as in the third stage the disk has already been exhausted. The upper dashed line indicates the current rotation period of the WD.
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Disk mass, M  d , and mass loss, M loss, as a function of the binary mass ratio, q. The solid curve represents the solutions for J1901+1458 (M = 1.35 M ⊙, P 0 = 3.14 s, ﹩\dot{M}=8.0\times {10}^{-7}{M}_{\odot }﹩ yr−1), while the dashed horizontal line shows the corresponding value used in the simulation.
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Disk mass, M  d , and mass loss, M loss, as a function of the binary mass ratio, q. The solid curve represents the solutions for J2211+1136 (M = 1.27 M ⊙,  P 0 = 3.14 s, ﹩\dot{M}=2.62\times {10}^{-7}{M}_{\odot }﹩ yr−1), while the dashed horizontal line shows the corresponding value used in the simulation.
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Predicted range of the primary and secondary mass. The solid curve represents the solutions for J2211+1136 (postmerger WD mass of M = 1.27 M ⊙, P 0 = 3.14 s, and ﹩\dot{M}=2.62\times {10}^{-7}{M}_{\odot }﹩ yr−1) and the dashed curve for J1901+1458 (postmerger WD mass of M = 1.35 M ⊙, P 0 = 3.14 s, and ﹩\dot{M}=8.0\times {10}^{-7}{M}_{\odot }﹩ yr−1).
Paper: The Double White Dwarf Merger Progenitors of SDSS J2211+1136 and ZTF J1901+1458
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, S. O. Kepler, J. A. Rueda
Figure caption: Accretion rate as a function of cooling age calculated from Equation (24) for J1901+1458. The WD parameters are M = 1.35 M ⊙, R = 2.14 × 108 cm, P 0 = 3.14 s, and P obs = 416.2 s. The magnetic field strength is B = 800 MG and θ = 90°.
Paper: Quasiperiodic Erupters: A Stellar Mass-transfer Model for the Radiation
Authors: Julian H. Krolik, Itai Linial
Figure caption: Schematic diagram of mass transfer. The star (blue disk) follows an eccentric orbit around the black hole (black disk). During the flare, its atmosphere expands outward on the side facing the black hole (dense blue shading; see Section 4). Gas from the atmosphere (lighter blue shading) streams through the L1 point, threaded by magnetic field (brown curves). After losing angular momentum, the gas follows a more eccentric orbit that takes it close enough to the black hole to suffer sizable apsidal precession. It shocks (dense red shading) against later-arriving gas and emits X-rays (green arrows). Deflected postshock gas cools rapidly (fainter red shading).
Paper: Quasiperiodic Erupters: A Stellar Mass-transfer Model for the Radiation
Authors: Julian H. Krolik, Itai Linial
Figure caption: Zoomed-in schematic diagram of the shocks and radiation region, showing only gas participating in the shocks. Newly arriving matter (blue shading and arrow) encounters matter whose orbit has been apsidally rotated (green shading and arrow). A pair of oblique shocks form (purple lines). Shock-heated gas (red shading) follows a deflected trajectory while radiating and cooling. Its width h and cooling length H ≡ ξ v  s  t cool are shown with double-headed arrows.
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: IR luminosity integrated over the wavelength range of 8–1000 μm, L IR, vs. CO(6–5) luminosity in units of K km s−1 pc2, ﹩L{{\prime} }_{\mathrm{CO}}﹩. The red circle is our ALMA result for a luminous LBG at z = 6, J0235–0532, whose CO(6–5) emission shows the 4σ significance level, with L IR and ﹩L{{\prime} }_{\mathrm{CO}}﹩ in the case of T dust = 50 K (Hashimoto et al. 2019; Harikane et al. 2020b). The upper error bar along the y-axis for J0235–0532 considers the case of a higher dust temperature of T dust = 80 K. The red triangle and diamond are also our ALMA results for the other luminous LBGs at z = 6, J1211–0118 and J0217–0208, respectively, which show no significant CO(6–5) detection. The red arrows correspond to the 3σ upper limits. The orange squares are high-z DSFGs (Riechers et al. 2010; Strandet et al. 2017; D’Odorico et al. 2018; Apostolovski et al. 2019; Casey et al. 2019) and the magenta diamonds are high-z quasars (Wang et al. 2010, 2011, 2016; Venemans et al. 2017a; Carniani et al. 2019) at z ∼ 5–7. The black triangles are nearby galaxies, Seyfert galaxies, and (U)LIRGs at low redshifts (z < 0.1) compiled by Liu et al. (2015).
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Top: dense gas fraction (I dense/I CO) derived from HCN (circles) and HCO+ (triangles) within the three apertures shown in Figure  9. The x-axis, d maj, corresponds to the distance of the aperture center along the galaxy major axis (in the direction of the leading edge). Bottom: HCN-HCO+ line ratio within the three apertures shown in Figure  9. In both panels the data points are colored by the average sSFR in each aperture and the error bars are a combination of random error derived from bootstrap resampling and a 5% calibration uncertainty assumed for each line flux (ALMA Band 3; ALMA Technical Handbook).
Paper: ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at z = 6.0293–6.2037
Authors: Yoshiaki Ono, Seiji Fujimoto, Yuichi Harikane, Masami Ouchi, Livia Vallini, Andrea Ferrara, Takatoshi Shibuya, Andrea Pallottini, Akio K. Inoue, Masatoshi Imanishi, Kazuhiro Shimasaku, Takuya Hashimoto, Chien-Hsiu Lee, Yuma Sugahara, Yoichi Tamura, Kotaro Kohno, Malte Schramm
Figure caption: Left: dust continuum SEDs of our z = 6 luminous LBGs, J1211–0118, J0235–0532, and J0217–0208 from top to bottom. The red arrows are the 3σ upper limits on the flux densities obtained in our ALMA observations. The black circles and downward arrows denote the observed flux densities and 3σ upper limits, respectively, obtained in Harikane et al. (2020b). The black solid curve indicates the best-fit modified blackbody and the gray shade corresponds to the 1σ uncertainties. Right: error contours for the two parameters L IR and T dust in the modified blackbody fitting. The dark and light shades denote the 1σ and 2σ confidence regions, respectively. The black cross corresponds to the best-fit parameters.
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Integrated intensity maps of HCN and HCO+ for IC3949. The solid contour shows the extent of the CO emission in IC3949, the cross marks the optical galaxy center, and the filled circle shows the FWHM beam size.