adsabs/AstroCLIMB huggingface dataset:
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: Comparison of the subgroups for each TESS orbit. The top figures are for Sector 24 and bottom Sector 25, with orbit 1 on the left for both sectors. The red line is the first subgroup while the green line marks the final for each orbit. The blue line indicates when the maximum shifts from the hump near ϕ = 0.55 to the maximum near ϕ = 0.75. The heavy black line marks the maximum (minimum) for each subgroup.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption:  V-magnitude observations of LS Her. The red lightcurves include data at maximum light while the green lightcurves include data at minimum light. The modeled data is shown in black and is extrapolated from the TESS/Wils model. We have scaled the model data to more closely match the V magnitude.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: TESS data from Sectors 24 and 25. The BE is clearly seen to change from one Blazhko cycle to the next with the amplitude of the BE growing with each successive cycle. The color coding indicates each TESS orbit.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: The peak-to-peak amplitude variations as a function of BJD for Sectors 24 and 25. The color coding is split by TESS orbits. The amplitude was measured from the fitting of the 0.5 day segments described in the text.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: The upper panel shows the model data (black) using the Wils et al. (2008) modulation frequencies and the TESS data (red) for s24o2, s25o1 and s25o2. This data was fit with the frequencies held constant. The lower panel shows the comparison between s24o1 and the extrapolated model data. The s24o1 data was not used in the model fit.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: Our modeled data shown over the course of 275 days, or 2.5 modulation cycles. The modulated Blazhko amplitude variations can be readily seen. Careful inspection shows the rise of a secondary hump which can destructively interfere with the Blazhko cycle, minimizing the Blazhko amplitude.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: The Fourier spectrum from TESS data after prewhitening of the primary frequency and higher harmonics. The Blazhko sidebands are promenient near the primary and 2nd harmonic peaks. The right panel shows modulation peaks after prewhitening the Blazhko sidebands.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: A phase-amplitude diagram showing the changes from one TESS orbit to the next. The arrows show the direction of the temporal changes which are counterclockwise in all cases.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: Comparison between the model data and the TESS data from Sector 51. As in Figure 3, the TESS data is shown in green and the extrapolated model data is in black. The comparison shows an incredibly close match.
Paper: Modulation of the Blazhko Cycle in LS Her
Authors: Ronald Wilhelm, Kenneth Carrell, Hannah H. Means, Adam Popowicz, Krzysztof Bernacki, Mariusz Frąckiewicz, Marek Szczepański, Adam Dustor, Jaylon Lockett, Jill Taylor, Stasha Youngquist
Figure caption: Comparison of Sector 51 data (green) and the modeled data from Sectors 24 and 25 (black). There is a time misalignment and a less than satisfactory amplitude match with the second orbit amplitude being much smaller than the model data.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Deep Hα+[S II] image obtained at the Subaru 8 m telescope shows the central part of L1630 with identifications of objects discussed in the text. HH 24 is the cluster of jets emanating from the multiple system SSV 63, while HH 19, 20, 21, 27, 37, and 70 are distant bow shocks related to the HH 24 jets. HH 22 is driven by an embedded source and HH 23 possibly by V1647 Ori. HH 25 and 26 are driven by embedded sources south of SSV 61. The height of the figure corresponds to approximately 1.5 pc. Star formation occurs along a narrow ridge oriented north–south with a length of ∼1 pc and a total mass around 230 M ⊙. Coordinates are equinox 2000.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: HST multifilter image with the protostellar components of the SSV 63 multiple system superposed (red circles). The red circle at the bottom of the figure marks the location of the embedded source HOPS 317, which illuminates an outflow cavity and drives the HH 24L flow. The filters used are: F814W (I band) as blue, F814W+F160W as green, F160W (H band) as orange, and F164N ([Fe II]) as red. This mixture of narrowband and wide-band images render jets, clouds, and outflow cavities particularly well. Color image courtesy is from Judy Schmidt/NASA/ESA. The F814W image is from HST program 9160 (PI D. Padgett), and the F160W image is from program 11548 (PI S.T. Megeath). The [Fe II] image is from this paper.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: VLA X-band maps of the five main sources of SSV 63. A possible companion to Wb is seen, as well as filamentary structure linked to Wa. The Ea source shows a radio jet along the axis of the E/C jet pair, and an orthogonal stubby bipolar structure. Positions and flux densities are given in Table 5. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: (Top) H2 HST image of the SSV 63 multiple system. The deeply embedded mid-infrared source Eb is not detectable at 2.1 μm, but is marked with an asterisk. Archival image was obtained with NICMOS (Program 11205, PI Muzerolle). (Bottom) A color composite of an HST [Fe II] image, an HST H-band image (Program 11548, PI Megeath), and an ALMA 1.3 mm continuum image. The circumstellar disks are clearly resolved, and it is seen that the near-infrared source Wb is not a star, but the compact NW lobe of a bipolar reflection nebula on either side of a silhouette disk (marked with white lines). North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The HH 24 complex (top) and SSV 61 reflection nebula (bottom) as seen in a color mosaic from Gemini composed of ﹩g^{\prime} ﹩ (blue), ﹩r^{\prime} ﹩ (cyan), ﹩i^{\prime} ﹩ (orange), Hα (red), and [S II] (blue). Color figure was prepared by Travis Rector. The figure is ∼4′ × 5′, corresponding to about 0.5 pc wide. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Annotated Hα–[S II] image obtained at the Subaru telescope showing the individual jets from SSV 63. The labels preserve and expand existing nomenclature. The multiple system is shown as red circles. White is [S II]-strong, black is Hα-strong. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: An H2 image obtained at the Gemini-N telescope showing the faint source S just south of the east and west binaries together with a weak detection of the embedded source NE. Together with the ALMA-detected source N, SSV 63 thus constitutes at least a septuple stellar system. A complex of H2 knots is seen between knots Wa and Ea. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Triptych of WFC3 HST images showing the HH 24 jet E and jet C in the Hα 6563 Å, [S II] 6717/31 Å, and [Fe II] 1.644 Å lines. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: GNIRS spectra of SSV63 Ea and Wb. Source Ea shows a heavily reddened continuum with a few emission lines and the CO bands in emission and no absorption features. In contrast, source Wb shows little reddening but a forest of molecular and atomic hydrogen lines, together with [Fe II], indicative of shocked outflow. Spectral regions with poor atmospheric transmission are omitted.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Spitzer 8 μm image of the SSV 63 multiple system. The source Eb is clearly resolved from Ea. The figure is about 40″ across. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: (Top) Detail of Figure 4 showing the bright bow shock HH 24A, located at the intersection of two flows originating from the embedded sources Ea and HOPS 317. The well-collimated jet HH 24E launched from the Class I source Ea impacts a cloud edge (seen well in Figure 4) and partly burrows through the cloud to reemerge farther down in a slightly different direction. (Bottom) An Hα-[S II] difference image of HH 24A, with Hα black and [S II] white. The little group of faint [S II]-bright knots to the left of the red dashed line moves approximately along the jet-E axis toward the SSE with about 40–50 km s−1 and evidently form part of this outflow. The bright central region of HH 24A is stationary, while the western extension is either stationary or has at most a slight motion toward the west. The dotted arrow indicates the direction from HOPS 317. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Jet J in an [S II] image taken with HST and WFC3. The jet emanates from the source Wb, which is deeply embedded and only detected at millimeter and centimeter wavelengths. The object seen at optical and infrared light is a combination of shocks and reflected light. The source drives a very faint but highly collimated jet toward the northwest and pointing to the large HH 19 bow shock. The southeast lobe is bent slightly southwards, and points to the bright HH 27 bow shock. The locations of the embedded sources Wb and Wa are marked with red lines. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Difference between the 2014 (black) and 2016 (white) HST [Fe II] images, showing the motion of the jet knots, seen especially clearly in the E and C jets. Note the ∼5° change in position angle of the southeastern portion of the E-jet. Substantial variability in the reflection nebulae appears as black and white pairs of nebulosity. Three parallel line-segments running from upper left to lower right are artifacts. North is up, and east is left. The figure is about 55″ wide.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: A superposition of an Hα (blue), an [S II] (green), and a 2.12 μm molecular hydrogen (red) image of the HH 24 complex obtained at the APO 3.5 m telescope. The figure is 2.′5 wide.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Structure of the E jet, based on the HST [Fe II] image in two cuts. Note that 5″ corresponds to 2000 au. The panel shows jet E emanating from the Ea source. Knot A is the large bright knot at the bottom. Individual knots in the E jet are numbered; see the text for details.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: (Top) A tracing of the HH 24E-jet from the [Fe II] HST image. Knots are identified with the nomenclature defined in Figure 13. (Bottom) The FWHMs of the individual knots of the E-jet within the first 20″ (8000 au) of the source were calculated by subtracting in quadrature the point-spread function.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Proper motions based on two epochs of HST images superposed on an Hα HST image. The 300 km s−1 velocity vector is about 11″ long and shows the motion in about 75 yr.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The C jet in two ground-based [S II] images taken in 2006 at Subaru and in 2021 at APO. The emergence of two bright knots from behind a cloud edge, indicated by the dotted line, is clearly seen. The motion of the jet during the 15 yr between exposures is indicated.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Structure of the C jet, based on the HST [Fe II] image in two cuts. Note that 5″ corresponds to 2000 au.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: HST near-infrared [Fe II] image of the HH 24 jet G. The tip of the jet (a1) falls outside the WFC3 field, but is seen as the top of the jet in Figure 20. This complex outflow consists of a central collimated jet (a1–a5) and two bright bow shocks (b and c) all wrapped within a wide outflow cavity whose sides are outlined in [Fe II] emission. Knot D was originally so designated by Herbig (1974), but has turned out to be an Hα-bright reflection nebula illuminated by the embedded VLA source NE. The bright lower part of the figure is shown with a different cut. The height of the figure is about 70″.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Three-color image showing “high-velocity” J = 3-2 CO emission associated with the parsec-scale outflows from the SSV 63 cloud core and the HH 24 jets. V lsr = 0–5 km s−1 is shown in blue; V lsr = 5–7.5 km s−1 is shown in green; and V lsr = 15–20 km s−1 is shown in red. The various HH objects that may be associated with the extended outflows from SSV 63 are marked. Dashed blue lines show the blueshifted HH components associated with jets C and J. Dashed red lines show redshifted components associated with their counterflows. North is up, and east is left. Data is from Stanke et al. (2022).
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Jet G in the optical in two different cuts, illustrating the brighter interior and fainter exterior structures. Each figure is the sum of deep Hα and [S II] images obtained at the Subaru 8 m telescope. The vertical dimension is 84″ corresponding to 0.16 pc. The apex of the jet is denoted a1, and more features are labeled in Figure 21.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The two fractured giant bow shocks driven by the two jets C (axis shown in green) and J (axis blue) shown in an Hα–[S II] image obtained with the Subaru telescope. Black is Hα-strong, and white is [S II]-strong. The two arrows mark defects in the CCD. The box indicates the area shown in Figure 23. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The HH 27 shock is a counterpart to the HH 19 terminal bow shock for the HH 24J jet. Farther south, a filamentary shock, here labeled HH 24 SSE, is located. Even farther south, two faint nebulosities, labeled HH 24 SSE2e and SSE2w, are found. The figure is a composite from Spitzer IRAC1 and IRAC2 images.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: A large complex of shocks is found north of HH 24. The group HH 20, 21, 37, 70 forms a giant fractured bow shock. Farther north, a distant faint shock is detected, here labeled NNW. The projected distance from source EA to the most distant shock HH 24 NNW is 1.45 pc. These shocks are associated with the HH 24C jet that is pointing toward them. HH 19 is a giant bow shock associated with the HH 24J jet. This figure is based on Hα (black) and [S II] (white) Subaru images.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Optical images of distant shocks in the HH 24 complex. Top: HH 24 NNW, which is a low-excitation object, in an [S II] image. Bottom: HH 24 SSE, which is a high-excitation object, in Hα. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Distant bow shocks HH 19, HH 21, and HH 37 from an Hα image obtained with the HST as a parallel ACS observation. The annotation of HH 19 is from Mundt et al. (1984). North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: Herschel 70 μm image of the HH 24 source SSV 63 and HH 24 MMS. At 70 μm the two sources HOPS 317 and MMS VLA 1 are just resolved, but at 160 μm the two sources are unresolved. The width of the figure is 85″.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The cloud core in which the HH 24 multiple system is embedded and its surroundings are seen here in a 850 μm dust continuum image from SCUBA2, courtesy of Helen Kirk (see Kirk et al. 2016). The components Wa/b, Ea/b, and NE are marked in red, as is HH 24 MMS to the south, while the five optically visible Hα emission stars are marked in green. Note how the multiple system is associated with a very dense core, while the Hα emission stars are located far from any dense cloud cores. The dimensions of the figure are 0.46 × 0.51 pc. North is up, and east is left.
Paper: The HH 24 Complex: Jets, Multiple Star Formation, and Orphaned Protostars
Authors: Bo Reipurth, J. Bally, Hsi-Wei Yen, H. G. Arce, L.-F. Rodríguez, A. C. Raga, T. R. Geballe, R. Rao, F. Comerón, S. Mikkola, C. A. Aspin, J. Walawender
Figure caption: The borderline brown dwarf Hα 5 moves away from the SSV 63 multiple system with a tangential velocity of about 26 km s−1. At this speed, it was ∼5800 yr ago close to the NE source, from which it was likely ejected in a triple interaction. The dotted lines represent a 2σ error on the Gaia measurement. The image is a sum of an Hα and an [S II] exposure with the Subaru telescope.