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Ring structure and warp of NGC5907 -- Interaction with dwarf galaxies
Astrophysics · Submitted 30 Jun 1998
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These results, coupled with the finding by others that dwarf galaxies tend to be found around giant galaxies, suggest that tidal interaction with companions, even if containing a mere 1% of the mass of the parent galaxy, might be sufficient to excite the warps found in the disks of many large spiral galaxies.
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The abstract, sentence by sentence
The edge-on, nearby spiral galaxy NGC5907 has long been used as the prototype of a ``non-interacting'' warped galaxy. We report here the discovery of two interactions with companion dwarf galaxies that substantially change this picture. First, a faint ring structure is discovered around this galaxy that is likely due to the tidal disruption of a companion dwarf spheroidal galaxy. The ring is elliptical in shape with the center of NGC5907 close to one of the ring's foci. This suggests the ring material is in orbit around NGC5907. No gaseous component to the ring has been detected either with deep H$\alpha$ images or in Very Large Array (VLA) HI 21-cm line maps. The visible material in the ring has an integrated luminosity <= 10^8 L_sun and its brightest part has a color R-I ~ 0.9. All of these properties are consistent with the ring being a tidally-disrupted dwarf spheroidal galaxy. Second, we find that NGC5907 has a dwarf companion galaxy, PGC54419, projected to be only 36.9 kpc from the center of NGC5907, close in radial velocity (\Delta V = 45 km s^{-1}) to the giant spiral galaxy. This dwarf is seen at the tip of the HI warp and in the direction of the warp. Hence, NGC5907 can no longer be considered ``non-interacting,'' but is obviously interacting with its dwarf companions much as the Milky Way interacts with its dwarf galaxies. These results, coupled with the finding by others that dwarf galaxies tend to be found around giant galaxies, suggest that tidal interaction with companions, even if containing a mere 1% of the mass of the parent galaxy, might be sufficient to excite the warps found in the disks of many large spiral galaxies.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The edge-on, nearby spiral galaxy NGC5907 has long been used as the prototype of a ``non-interacting'' warped galaxy. | background 1.00 | 0.04 | 0.02 | asserted 1.00 |
| s1 | We report here the discovery of two interactions with companion dwarf galaxies that substantially change this picture. | contribution 0.78 | 0.95 | 0.34 | asserted 1.00 |
| s2 | First, a faint ring structure is discovered around this galaxy that is likely due to the tidal disruption of a companion dwarf spheroidal galaxy. | result 0.96 | 0.95 | 0.12 | hedged possibility 0.90 |
| s3 | The ring is elliptical in shape with the center of NGC5907 close to one of the ring's foci. | result 1.00 | 0.86 | 0.02 | asserted 1.00 |
| s4 | This suggests the ring material is in orbit around NGC5907. | interpretation 0.99 | 0.71 | 0.03 | hedged possibility 0.96 |
| s5 | No gaseous component to the ring has been detected either with deep H$\alpha$ images or in Very Large Array (VLA) HI 21-cm line maps. | result 0.97 | 0.91 | 0.02 | asserted 1.00 |
| s6 | The visible material in the ring has an integrated luminosity <= 10^8 L_sun and its brightest part has a color R-I ~ 0.9. | result 1.00 | 0.87 | 0.02 | asserted 1.00 |
| s7 | All of these properties are consistent with the ring being a tidally-disrupted dwarf spheroidal galaxy. | interpretation 0.99 | 0.76 | 0.09 | hedged possibility 0.97 |
| s8 | Second, we find that NGC5907 has a dwarf companion galaxy, PGC54419, projected to be only 36.9 kpc from the center of NGC5907, close in radial velocity (\Delta V = 45 km s^{-1}) to the giant spiral galaxy. | result 0.99 | 0.96 | 0.06 | asserted 1.00 |
| s9 | This dwarf is seen at the tip of the HI warp and in the direction of the warp. | result 0.95 | 0.89 | 0.05 | asserted 1.00 |
| s10 | Hence, NGC5907 can no longer be considered ``non-interacting,'' but is obviously interacting with its dwarf companions much as the Milky Way interacts with its dwarf galaxies. | interpretation 0.99 | 0.83 | 0.79 | asserted 1.00 |
| s11 | These results, coupled with the finding by others that dwarf galaxies tend to be found around giant galaxies, suggest that tidal interaction with companions, even if containing a mere 1% of the mass of the parent galaxy, might be sufficient to excite the warps found in the disks of many large spiral galaxies. | interpretation 1.00 | 0.26 | 0.47 | speculative 0.67 |
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The paper
Original abstract
The edge-on, nearby spiral galaxy NGC5907 has long been used as the prototype of a ``non-interacting'' warped galaxy. We report here the discovery of two interactions with companion dwarf galaxies that substantially change this picture. First, a faint ring structure is discovered around this galaxy that is likely due to the tidal disruption of a companion dwarf spheroidal galaxy. The ring is elliptical in shape with the center of NGC5907 close to one of the ring's foci. This suggests the ring material is in orbit around NGC5907. No gaseous component to the ring has been detected either with deep H$\alpha$ images or in Very Large Array (VLA) HI 21-cm line maps. The visible material in the ring has an integrated luminosity <= 10^8 L_sun and its brightest part has a color R-I ~ 0.9. All of these properties are consistent with the ring being a tidally-disrupted dwarf spheroidal galaxy. Second, we find that NGC5907 has a dwarf companion galaxy, PGC54419, projected to be only 36.9 kpc from the center of NGC5907, close in radial velocity (\Delta V = 45 km s^{-1}) to the giant spiral galaxy. This dwarf is seen at the tip of the HI warp and in the direction of the warp. Hence, NGC5907 can no longer be considered ``non-interacting,'' but is obviously interacting with its dwarf companions much as the Milky Way interacts with its dwarf galaxies. These results, coupled with the finding by others that dwarf galaxies tend to be found around giant galaxies, suggest that tidal interaction with companions, even if containing a mere 1% of the mass of the parent galaxy, might be sufficient to excite the warps found in the disks of many large spiral galaxies.
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