adsabs/AstroCLIMB huggingface dataset:
Paper: A JWST MIRI MRS View of the η Tel Debris Disk and Its Brown Dwarf Companion
Authors: Yiwei Chai, Christine H. Chen, Kadin Worthen, Alexis Li, Antranik A. Sefilian, William Balmer, Dean C. Hines, David R. Law, B. A. Sargent, Mark Wyatt, Cicero X. Lu, Marshall D. Perrin, Isabel Rebollido, Emily Rickman, G. C. Sloan
Figure caption: MIRI MRS collapsed subband images of η Tel B from 3A to 4C using a logarithmic scaling. We obtain a 3σ–10σ detection of the brown dwarf across 3A–3C and a 3σ detection in 4A. In subbands 4B and 4C, increased background noise renders the companion irrecoverable; for this reason, we omit these two subbands in our spectral extraction of the brown dwarf. The black circle indicates the size of the extraction aperture.
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: (a) CDFs illustrating the X-ray flare energy distributions for the 2003 epoch (in black) and later (2012, 2016, and 2023) epochs (in color). The bright end of the 2003 epoch CDF is fitted with the Pareto (power-law) function (red), with a slope of β = 0.91. (b)–(d) Scatter plots depicting the energies of X-ray flares observed during the 2003 epoch (in black) and subsequent epochs (in red), plotted against stellar mass, stellar surface area, and SED IRAC slope. Corresponding legends present the τ coefficients and p-values obtained from Kendall’s τ test. (e)–(f) Depiction of guiding trends: the peak plasma temperature and flare loop scale as functions of X-ray flare energy, based on the COUP flare sample and flare quantities from K. V. Getman et al. (2008a). The purple curves represent spline fits to the 25%, 50%, and 75% quartiles of the distributions, created using R’s Constrained B-Splines cobs function (P. T. Ng & M. Maechler 2007).
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: (a)–(c) Comparison of stellar X-ray characteristic luminosities across different epochs. The unity lines are depicted in red. Linear regression fits using the Major Axis algorithm within R’s lmodel2 function are shown in green. Figure legends list the intercept, slope, and half-widths of the 95% confidence intervals inferred by lmodel2. (d)–(f) Long-term X-ray characteristic variability amplitude (A) plotted against χ 2, stellar mass, and SED IRAC slope for the entire stellar sample. Stars with the highest statistically reliable A are highlighted with red points. Figure legends provide coefficients and p-values from Kendall’s τ test. (g)–(h) Similar to panels (d)–(e), but for the subset of diskless stars. Diskless stars with the highest statistically reliable A are denoted with green points. (i) For diskless stars, amplitude A plotted against stellar rotation velocity.
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: Examples of X-ray light curves presented in units of intrinsic stellar X-ray luminosity for select targets observed with HET-HPF, ALMA, and VLBA. For further details, consult the caption of Figure 3. Refer to the next page for the continuation of the figure.
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: Comparison of the observed X-ray characteristic variability amplitude A (black) for our sample of 87 diskless PMS stars (shown in Figure 6(g)), with the A app results from simulations (described in the text) assuming intrinsic cyclic activity periods of 1 yr (blue), 5 yr (red), and 10 yr (green) and an intrinsic variability amplitude ﹩{A}_{\mathrm{intr}}=1.7﹩. The p-values from the AD test for these comparisons are provided in the figure legend.
Paper: Multi-Observatory Research of Young Stellar Energetic Flares (MORYSEF): X-Ray-flare-related Phenomena and Multi-epoch Behavior
Authors: Konstantin V. Getman, Eric D. Feigelson, Abygail R. Waggoner, L. Ilsedore Cleeves, Jan Forbrich, Joe P. Ninan, Oleg Kochukhov, Vladimir S. Airapetian, Sergio A. Dzib, Charles J. Law, Christian Rab
Figure caption: Bivariate relationship between early (epoch 2003) and late (epochs 2012, 2016, and 2023) flares for Orion Nebula PMS stars. If multiple flares are seen in more than one later epoch, the weaker flare is shown. The dashed red line shows equal luminosities in early and late epochs.
Paper: Thermal Evolution of the Intergalactic Medium due to Lyα Photons during the Cosmic Dawn
Authors: Janakee Raste, Anjan Kumar Sarkar, Shiv K. Sethi
Figure caption: This figure explores the approach from the flat to the tilted profile on the thermal evolution of the IGM. It corresponds to Lyα continuum + 20% injected photons at z = 20 and initial temperature T = 10 K. As in Figure 3, we model the approach to tilted profile by assuming ﹩{x}_{\max }\ll {10}^{5}﹩. In the left panel, we start with the tilted profile from t = 0. In the middle panel, we start with a flat profile, and the tilt starts at after 1 Myr. In the right panel, we show the comparison of evolution of temperature with time in these two cases, along with the flat profile case (right panel of Figure 5; dotted curves). The dashed (solid) curves correspond to thermal evolution for intensity profiles of left (middle) panel. The temperature in all three cases reach equilibrium with dotted curves (which follow the solid curves for t ≲ 1 Myr) having the highest temperature and the dashed curves with the lowest temperature. A comparison between dotted and solid curves shows that the heating rate is lower for a tilted profile, which is further underlined by dashed curves for which the tilted profile is switched on at t = 0.
Paper: Thermal Evolution of the Intergalactic Medium due to Lyα Photons during the Cosmic Dawn
Authors: Janakee Raste, Anjan Kumar Sarkar, Shiv K. Sethi
Figure caption: In the left and middle panels, we show the evolution of photon intensity profile for the continuum + 20% injected photons case at redshift z = 20 with an initial temperature T = 10 K and ﹩C={10}^{-12}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}\,{\mathrm{sr}}^{-1}﹩. In the left panel, the source switches on at t = 0; while in the middle panel, the initial profile is assumed to have quasi-static form, and it switches off at t = 0. The middle panel shows that, when the source is switched off, the injected feature redshifts out of the resonance much faster than the continuum feature. Therefore, this scenario heats up the gas (see the middle and right panel of Figure 2 for comparison). In the right panel, we show the evolution of temperature for different injected photon fractions and compare it with the continuum photon only case. We see here that the temperature of the gas reaches different equilibrium values for different injected photons' fraction for the same value of C.
Paper: WTP 19aalnxx: Discovery of a Bright Mid-infrared Transient in the Emerging Class of Low-luminosity Supernovae Revealed by Delayed Circumstellar Interaction
Authors: Charlotte Myers, Kishalay De, Lin Yan, Jacob E. Jencson, Nicholas Earley, Christoffer Fremling, Daichi Hiramatsu, Mansi M. Kasliwal, Ryan M. Lau, Morgan MacLeod, Megan Masterson, Christos Panagiotou, Robert Simcoe, Samaporn Tinyanont
Figure caption: The discovery location and multiwavelength light curve of WTP 19aalnxx. Left panels: multicolor optical (gri) preexplosion image from the Pan-STARRS1 (PS1) survey (top), postexplosion late-time r-band imaging using the Southern Astrophysical Research (SOAR, middle), and postexplosion late-time K-band imaging using the P200 (bottom). Middle panels: science, reference, and difference WISE imaging triplet of the location of WTP 19aalnxx showing the detection of an MIR transient. Right panel: multiwavelength light curve of WTP 19aalnxx from NEOWISE, PS1, Asteroid Terrestrial-impact Last Alert System (ATLAS), and Zwicky Transient Facility (ZTF) surveys. Solid symbols denote detections in the respective band while hollow symbols with downward arrows indicate upper limits. The NEOWISE photometry is available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: WTP 19aalnxx: Discovery of a Bright Mid-infrared Transient in the Emerging Class of Low-luminosity Supernovae Revealed by Delayed Circumstellar Interaction
Authors: Charlotte Myers, Kishalay De, Lin Yan, Jacob E. Jencson, Nicholas Earley, Christoffer Fremling, Daichi Hiramatsu, Mansi M. Kasliwal, Ryan M. Lau, Morgan MacLeod, Megan Masterson, Christos Panagiotou, Robert Simcoe, Samaporn Tinyanont
Figure caption: Comparison of the late-time spectra of WTP 19aalnxx to other known SNe exhibiting late-time CSM interaction. Top panel: the late-time optical spectrum compared to other known interacting SNe spanning different spectroscopic types at peak light—the Type IIb SN 2020jfv (J. Sollerman et al. 2021); Type IIn SN 2015da (L. Tartaglia et al. 2020); Type Ib SN 2019oys (J. Sollerman et al. 2020), SN 2014C (B. P. Thomas et al. 2022), SN 2004dk (D. Pooley et al. 2019); Type Ia SN 2011km/PTF 11kx (M. L. Graham et al. 2017); and Type Ia-CSM (SN 2020uem; Y. Sharma et al. 2023). Bottom: NIR spectrum of WTP 19aalnxx compared to our Magellan/FIRE follow-up of two additional optically discovered SNe exhibiting late-time MIR brightening—the Type IIb SN 2020jfv and Type II SN 2020yzq. Regions of low atmospheric transparency have been masked with gray shaded areas.
Paper: Thermal Evolution of the Intergalactic Medium due to Lyα Photons during the Cosmic Dawn
Authors: Janakee Raste, Anjan Kumar Sarkar, Shiv K. Sethi
Figure caption: The temperature evolution is displayed for 5% (left), 10% (middle), and 20% (right) fraction of injected photons for initial temperature T K = 10 K and two redshifts. The solid curves are for z = 20, and dashed curves are for z = 15. For higher fraction of injected photons, the equilibrium temperature is lower. This final equilibrium temperature does not depend on the rate of energy injection C, but only on the ratio of the continuum to injected photons. It also does not depend on the initial temperature (we have not shown it here). The final temperature has a mild dependence on redshift, with lower temperature reached at smaller redshifts.
Paper: WTP 19aalnxx: Discovery of a Bright Mid-infrared Transient in the Emerging Class of Low-luminosity Supernovae Revealed by Delayed Circumstellar Interaction
Authors: Charlotte Myers, Kishalay De, Lin Yan, Jacob E. Jencson, Nicholas Earley, Christoffer Fremling, Daichi Hiramatsu, Mansi M. Kasliwal, Ryan M. Lau, Morgan MacLeod, Megan Masterson, Christos Panagiotou, Robert Simcoe, Samaporn Tinyanont
Figure caption: Best-fit models of the SED from the NIR to W2 band in 2022 obtained using DUSTY. We show the best-fit models for both silicate (denoted as Si) and graphite (denoted as C) dust compositions; the best-fit parameters for the two cases are shown in the text. For comparison, we also show a model fit corresponding to silicate dust with a fixed grain size of a = 0.1 μm, which provides parameters consistent with the silicate model with an MRN size distribution.
Paper: WTP 19aalnxx: Discovery of a Bright Mid-infrared Transient in the Emerging Class of Low-luminosity Supernovae Revealed by Delayed Circumstellar Interaction
Authors: Charlotte Myers, Kishalay De, Lin Yan, Jacob E. Jencson, Nicholas Earley, Christoffer Fremling, Daichi Hiramatsu, Mansi M. Kasliwal, Ryan M. Lau, Morgan MacLeod, Megan Masterson, Christos Panagiotou, Robert Simcoe, Samaporn Tinyanont
Figure caption: Comparison of the W2 light curve of WTP 19aalnxx to 4.5 μm light curves of different types of SNe observed with the Spitzer Space Telescope (T. Szalai et al. 2021). SNe of a given type are plotted with the same color (shown in the legend) while the evolution of each object is shown with connected symbols.
Paper: WTP 19aalnxx: Discovery of a Bright Mid-infrared Transient in the Emerging Class of Low-luminosity Supernovae Revealed by Delayed Circumstellar Interaction
Authors: Charlotte Myers, Kishalay De, Lin Yan, Jacob E. Jencson, Nicholas Earley, Christoffer Fremling, Daichi Hiramatsu, Mansi M. Kasliwal, Ryan M. Lau, Morgan MacLeod, Megan Masterson, Christos Panagiotou, Robert Simcoe, Samaporn Tinyanont
Figure caption: Modeling of the temporal evolution of the spectral energy distribution (SED) of WTP 19aalnxx. Left: modified blackbody fitting for three representative epochs (indicated in the legend) postexplosion for the optically thin silicate dust model. The solid circles mark the W1 and W2 fluxes used to perform the fit. Right: temporal evolution of the temperature and mass of dust inferred from fitting the NEOWISE MIR photometry (see text). The dashed lines show the expected dust mass in the case of collisional shock heating in the CDS, for two different shock velocities (O. D. Fox et al. 2010).
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: Integrated-intensity images (moment-0 maps) of selected molecular transitions: C18O, CO, CH3CHO, HCOOCH3, H2CO, CH3OH, OCS, 13CS, and H2S. The origin of the coordinate system is the 1.3 mm continuum peak at [α 2000, δ 2000] = [05h35m23.ˢ42, −05°01′30.″6], and the ranges of R.A. (x-axis) and decl. (y-axis) span ±2″. Each panel is labeled at the top with the corresponding chemical formula and the upper-energy level of the transition shown in color. The velocity ranges for integration are ±40 km s−1 for CO and SiO, ±3 km s−1 for 13CS, and ±7.5 km s−1 for others. The black dashed contours depict the 1.3 mm continuum, set at levels of [5, 10, 20, 40, 80, 160]σ, where σ corresponds to 0.9 mJy beam−1 (or 0.13 K in terms of brightness temperature). The orange ellipses located at the bottom-left corners indicate the beam sizes for the Cycle 6 ALMA program. The green contours display the SiO integrated-intensity map, highlighted at levels of [10, 25, 40]σ, where each σ corresponds to 28 mJy beam−1 km s−1. The distribution of the molecules in panels (e)–(i) are particularly noteworthy; these molecules are not typical outflow tracers but exhibit two-lobed distributions. The white crosses in panels (c) and (d) illustrate the peak position of the corresponding transition.
Paper: The Importance of Ambipolar Heating in the Standard Thin Accretion Disk with Outflows
Authors: Mahmoud Gholipour, Amir Abbas Eslami Shafigh
Figure caption: Latitudinal profile of temperature for n = 1.3, f = 0.01, and γ = 5/3, with two different values of α and Λ. Each panel is labeled with the corresponding value of the dimensionless AD Elsässer number for two cases of thermal effects: Γ = 0 (dashed line) and Γ ≠ 0 (solid line). Here, T 0 is the temperature of the midplane.
Paper: The Importance of Ambipolar Heating in the Standard Thin Accretion Disk with Outflows
Authors: Mahmoud Gholipour, Amir Abbas Eslami Shafigh
Figure caption: Latitudinal profile of radial velocity for n = 1.3, f = 0.01, and γ = 5/3, with two different values of α and Λ. The plots above display the outflow regions, with the vertical axis labeled as “v  r (θ),” being proportional to v  r /v  k , where v  k  represents the Keplerian velocity. The horizontal axis, labeled as “θ,” is measured in degrees.
Paper: The Importance of Ambipolar Heating in the Standard Thin Accretion Disk with Outflows
Authors: Mahmoud Gholipour, Amir Abbas Eslami Shafigh
Figure caption: Latitudinal profile of density for n = 1.3, f = 0.01, and γ = 5/3, with two different values of α and Λ. Each panel is labeled with the corresponding value of the dimensionless AD Elsässer number for two cases of thermal effects: Γ = 0 (dashed line) and Γ ≠ 0 (solid line).
Paper: The Importance of Ambipolar Heating in the Standard Thin Accretion Disk with Outflows
Authors: Mahmoud Gholipour, Amir Abbas Eslami Shafigh
Figure caption: Latitudinal profile of radial velocity for n = 1.3, f = 0.01, and γ = 5/3, with two different values of α and Λ. The plots above display the inflow regions, with the vertical axis labeled as “v  r (θ),” being proportional to v  r /v  k , where v  k  represents the Keplerian velocity. The horizontal axis, labeled as “θ,” is measured in degrees.
Paper: The Importance of Ambipolar Heating in the Standard Thin Accretion Disk with Outflows
Authors: Mahmoud Gholipour, Amir Abbas Eslami Shafigh
Figure caption: Latitudinal profile of azimuthal velocity for n = 1.3, f = 0.01, and γ = 5/3, with two different values of α and Λ. The vertical axis is labeled as “v  ϕ (θ)” and is proportional to v  r /v  k , where v  k  represents the Keplerian velocity. The horizontal axis, labeled as “θ,” is measured in degrees.
Paper: The Importance of Ambipolar Heating in the Standard Thin Accretion Disk with Outflows
Authors: Mahmoud Gholipour, Amir Abbas Eslami Shafigh
Figure caption: Latitudinal profile of ambipolar diffusivity for n = 1.3, f = 0.01, and γ = 5/3, with two different values of α and Λ. The vertical axis is labeled as “η 0/η(θ),” where η 0 represents the value of ambipolar diffusivity in the midplane. The horizontal axis, labeled as “θ,” is measured in degrees.
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: The PV diagrams of selected molecular transitions along the outflow axis (PA = –4° with the center at the 1.3 mm continuum peak). The relative position offset (Δp) is from south (Δp < 0″) to north (Δp > 0″). The upper-left label in each panel shows the chemical species and the upper energy E u of the transitions. Note that the diagrams are exported from the data cube of the full spectral window so the separated components may come from molecular transitions other than the labeled one in each label (e.g., the components at (−7.5 km s−1, 0″) in panel (h) and at (−7.5 km s−1, 0″) in panel (k)). The color maps and the brown contours are the PV diagram of the labeled transitions. The gray contours represent the CO PV diagram. The brown and gray contours are in steps of [5, 10, 15, 20, 25, 30, 40, 50, 60, 70, 80]σ. The navy polylines, referred from the PV diagram of the CH3OH 45 K transition, consists of two horizontal lines at Δp = 0.″3 and −0.″2 and a diagonal line moving from Δp = 0.″3 to −0.″2 at Δv = 0.75 km s−1 and −0.75 km s−1, respectively. The diagrams are exported by CARTA 4.0 (A. Comrie et al. 2021). The gap in CO indicates the missing flux at low velocities due to interferometry. The broadening of the velocity range localized at Δp = 0.″3 and −0.″2 is significant in CH3OH, H2CO, OCS, and H2S, and tentatively observed in 13CS. Additionally, the rapid growth of velocity Δv with position offset Δp described in C. Lee et al. (2001) is significant in SiO. These characteristics suggest that these molecules are also tracing jet-driven bow shocks (C. Lee et al. 2001).
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: The CH3OH 51,4 − 42,3 transition in Cycle 3 observations. The top and bottom rows show the images at the blue- and redshifted channels, respectively. The labels in each panel shows the relative velocity (Δv = v − v LSR). At Δv = 0 km s−1 the intensity map displays an arclike emission pattern west of the center with an absorption feature toward the continuum peak. At ∣Δv∣ > 0.68 km s−1, there is a single lobe (Δδ ∼0.″3) on each of the northern and the southern sides of the arc (Δδ ∼0.″2) seen at Δv = 0 km s−1.
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: PV diagrams cut along (panels (a), (c), and (e)) and across (panels (b), (d), and (f)) to the outflow axis for three selected frequency ranges. The x-axes are in terms of frequency. The origin of the y-axes is the continuum peak. The contours represent levels of [10, 20, 30, 40]σ. In panels (a) and (b), the typical outflowing gas tracer, SiO, is visible only in the cut along the outflow axis with a spur structure. Panels (c) and (d) show that COMs like HCOOCH3 and CH3OCH3 display a single peak in both diagrams. In panels (e) and (f), CH3OH and H2CO present a single peak in the cut across the outflow axis, accompanied by a two-lobe feature in the cut along the outflow axis.
Paper: ALMASOP. The Localized and Chemically Rich Features near the Bases of the Protostellar Jet in HOPS 87
Authors: Shih-Ying Hsu, Chin-Fei Lee, Sheng-Yuan Liu, Doug Johnstone, Tie Liu, Satoko Takahashi, Leonardo Bronfman, Huei-Ru Vivien Chen, Somnath Dutta, David J. Eden, Neal J. Evans, Naomi Hirano, Mika Juvela, Yi-Jehng Kuan, Woojin Kwon, Chang Won Lee, Jeong-Eun Lee, Shanghuo Li, Chun-Fan Liu, Xunchuan Liu, Qiuyi Luo, Sheng-Li Qin, Dipen Sahu, Patricio Sanhueza, Hsien Shang, 賢 尚, Kenichi Tatematsu, Yao-Lun Yang
Figure caption: Spectra of selected molecular transitions along the cavity axis. The labels at the right of each row show the formula and the upper energy of each transition. The labels at the top of each column show the angular offset from the continuum peak. The horizontal dashed lines represent the level of 5σ. In the panels of 13CS, the line at ∼–7 km s−1  is another molecular transition. The y-axis is the fraction of peak intensity. The north is blueshifted (coming toward us) and the south is redshifted (moving away), and the lines extend to bluer and redder velocities at the north and south positions, respectively.