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HST NICMOS Images of the HH 7/11 Outflow in NGC1333
Astrophysics · Submitted 28 Jul 2002
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The NICMOS high angular resolution observations confirm the nature of a small scale jet arising from SVS 13, and resolve a structure in the HH 7 working surface that could correspond to Mach disk H2 emission.
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The abstract, sentence by sentence
We present near infrared images in H2 at 2.12um of the HH 7/11 outflow and its driving source SVS 13 taken with HST NICMOS 2 camera, as well as archival Ha and [SII] optical images obtained with the WFPC2 camera. The NICMOS high angular resolution observations confirm the nature of a small scale jet arising from SVS 13, and resolve a structure in the HH 7 working surface that could correspond to Mach disk H2 emission. The H2 jet has a length of 430 AU (at a distance of 350 pc), an aspect ratio of 2.2 and morphologically resembles the well known DG Tau optical micro-jet. The kinematical age of the jet (approx. 10 yr) coincides with the time since the last outburst from SVS 13. If we interpret the observed H2 flux density with molecular shock models of 20-30 km/s, then the jet has a density as high as 1.e+5 cc. The presence of this small jet warns that contamination by H2 emission from an outflow in studies searching for H2 in circumstellar disks is possible. At the working surface, the smooth H2 morphology of the HH 7 bowshock indicates that the magnetic field is strong, playing a major role in stabilizing this structure. The H2 flux density of the Mach disk, when compared with that of the bowshock, suggests that its emission is produced by molecular shocks of less than 20 km/s. The WFPC2 optical images display several of the global features already inferred from groundbased observations, like the filamentary structure in HH 8 and HH 10, which suggests a strong interaction of the outflow with its cavity. The H2 jet is not detected in {SII] or Ha, however, there is a small clump at approx. 5'' NE of SVS 13 that could be depicting the presence either of a different outburst event or the north edge of the outflow cavity.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present near infrared images in H2 at 2.12um of the HH 7/11 outflow and its driving source SVS 13 taken with HST NICMOS 2 camera, as well as archival Ha and [SII] optical images obtained with the WFPC2 camera. | method 0.56 | 0.94 | 0.04 | asserted 0.97 |
| s1 | The NICMOS high angular resolution observations confirm the nature of a small scale jet arising from SVS 13, and resolve a structure in the HH 7 working surface that could correspond to Mach disk H2 emission. | result 0.95 | 0.94 | 0.37 | asserted 0.55 |
| s2 | The H2 jet has a length of 430 AU (at a distance of 350 pc), an aspect ratio of 2.2 and morphologically resembles the well known DG Tau optical micro-jet. | result 1.00 | 0.93 | 0.13 | asserted 1.00 |
| s3 | The kinematical age of the jet (approx. 10 yr) coincides with the time since the last outburst from SVS 13. | result 0.76 | 0.82 | 0.09 | asserted 0.99 |
| s4 | If we interpret the observed H2 flux density with molecular shock models of 20-30 km/s, then the jet has a density as high as 1.e+5 cc. | interpretation 0.52 | 0.82 | 0.07 | hedged possibility 0.69 |
| s5 | The presence of this small jet warns that contamination by H2 emission from an outflow in studies searching for H2 in circumstellar disks is possible. | interpretation 0.91 | 0.55 | 0.14 | hedged possibility 0.90 |
| s6 | At the working surface, the smooth H2 morphology of the HH 7 bowshock indicates that the magnetic field is strong, playing a major role in stabilizing this structure. | interpretation 0.98 | 0.82 | 0.13 | hedged possibility 0.82 |
| s7 | The H2 flux density of the Mach disk, when compared with that of the bowshock, suggests that its emission is produced by molecular shocks of less than 20 km/s. | interpretation 0.91 | 0.88 | 0.10 | hedged possibility 0.99 |
| s8 | The WFPC2 optical images display several of the global features already inferred from groundbased observations, like the filamentary structure in HH 8 and HH 10, which suggests a strong interaction of the outflow with its cavity. | result 0.91 | 0.72 | 0.05 | asserted 0.52 |
| s9 | The H2 jet is not detected in {SII] or Ha, however, there is a small clump at approx. 5'' NE of SVS 13 that could be depicting the presence either of a different outburst event or the north edge of the outflow cavity. | result 0.86 | 0.91 | 0.06 | hedged possibility 0.89 |
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The paper
Original abstract
We present near infrared images in H2 at 2.12um of the HH 7/11 outflow and its driving source SVS 13 taken with HST NICMOS 2 camera, as well as archival Ha and [SII] optical images obtained with the WFPC2 camera. The NICMOS high angular resolution observations confirm the nature of a small scale jet arising from SVS 13, and resolve a structure in the HH 7 working surface that could correspond to Mach disk H2 emission. The H2 jet has a length of 430 AU (at a distance of 350 pc), an aspect ratio of 2.2 and morphologically resembles the well known DG Tau optical micro-jet. The kinematical age of the jet (approx. 10 yr) coincides with the time since the last outburst from SVS 13. If we interpret the observed H2 flux density with molecular shock models of 20-30 km/s, then the jet has a density as high as 1.e+5 cc. The presence of this small jet warns that contamination by H2 emission from an outflow in studies searching for H2 in circumstellar disks is possible. At the working surface, the smooth H2 morphology of the HH 7 bowshock indicates that the magnetic field is strong, playing a major role in stabilizing this structure. The H2 flux density of the Mach disk, when compared with that of the bowshock, suggests that its emission is produced by molecular shocks of less than 20 km/s. The WFPC2 optical images display several of the global features already inferred from groundbased observations, like the filamentary structure in HH 8 and HH 10, which suggests a strong interaction of the outflow with its cavity. The H2 jet is not detected in {SII] or Ha, however, there is a small clump at approx. 5'' NE of SVS 13 that could be depicting the presence either of a different outburst event or the north edge of the outflow cavity.
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