[ITAL]Hubble Space Telescope[/ITAL] Proper-Motion Measurements of the η Carinae Nebula

Morse, Jon A.; Kellogg, James R.; Bally, John; Davidson, Kris; Balick, Bruce; Ebbets, Dennis

doi:10.1086/319092

Cited by 81 publications

(146 citation statements)

References 18 publications

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“…The far-infrared emission originates from the circumstellar dust envelope around η Car. The famous bipolar Homunculus Nebula is thought to be the result of the "Great Eruption" in the 1840's (see Smith et al 1998;Currie & Dowling 1999;Morse et al 2001;Smith 2005;Artigau et al 2011;Davidson & Humphreys 2012). The total dust + gas mass in the bipolar nebula and a dense equatorial torus in the Homunculus is estimated to be about 15−20 M (Morris et al 1999;Smith et al 2003).…”

Section: The Far-infrared Spectral Energy Distribution Of η Carinaementioning

confidence: 99%

Herschelfar-infrared observations of the Carina Nebula complex

Gaczkowski

Preibisch

Ratzka

et al. 2012

A&A

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Context. The Carina Nebula represents one of the largest and most active star forming regions known in our Galaxy. It contains numerous very massive (M > ∼ 40 M ) stars that strongly affect the surrounding clouds by their ionizing radiation and stellar winds. Aims. Our recently obtained Herschel PACS and SPIRE far-infrared maps cover the full area (≈8.7 deg 2 ) of the Carina Nebula complex (CNC) and reveal the population of deeply embedded young stellar objects (YSOs), most of which are not yet visible in the mid-or near-infrared. Methods. We study the properties of the 642 objects that are independently detected as point-like sources in at least two of the five Herschel bands. For those objects that can be identified with apparently single Spitzer counterparts, we use radiative transfer models to derive information about the basic stellar and circumstellar parameters. Results. We find that about 75% of the Herschel-detected YSOs are Class 0 protostars. The luminosities of the Herschel-detected YSOs with SED fits are restricted to values of ≤5400 L , their masses (estimated from the radiative transfer modeling) range from ≈1 M to ≈10 M . Taking the observational limits into account and extrapolating the observed number of Herschel-detected protostars over the stellar initial mass function suggest that the star formation rate of the CNC is ∼0.017 M /year. The spatial distribution of the Herschel YSO candidates is highly inhomogeneous and does not follow the distribution of cloud mass. Rather, most Herschel YSO candidates are found at the irradiated edges of clouds and pillars. The far-infrared fluxes of the famous object η Car are about a factor of two lower than expected from observations with the Infrared Space Observatory obtained 15 years ago; this difference may be a consequence of dynamical changes in the circumstellar dust in the Homunculus Nebula around η Car. Conclusions. The currently ongoing star formation process forms only low-mass and intermediate-mass stars, but no massive (M > ∼ 20 M ) stars. The characteristic spatial configuration of the YSOs provides support to the picture that the formation of this latest stellar generation is triggered by the advancing ionization fronts.

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Section: The Far-infrared Spectral Energy Distribution Of η Carinaementioning

confidence: 99%

Herschelfar-infrared observations of the Carina Nebula complex

Gaczkowski

Preibisch

Ratzka

et al. 2012

A&A

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“…This nebula, with an estimated mass ∼1M , consists of a two-lobe structure divided by a thin equatorial torus. Morse et al (2001) performed a proper motion study in this nebula by comparing HST images taken at three different epochs and concluded that the "Homunculus" also shows a single Hubble law and was formed in less that 10 yr during the great eruption in the 1840's. These measurements are only done in the plane of the sky (neither the position nor the velocities are derived along the line of sight, as in our case), so they do not depend on the orientation of the nebula or on the distance.…”

Section: The Origin Of the Ppn M 1-92mentioning

confidence: 99%

Minkowski's footprint revisited

Alcolea¹,

Neri

Bujarrabal

2007

A&A

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Context. M 1-92 can be considered an archetype of bipolar pre-planetary nebulae. It shows a clear axial symmetry, along with the kinematics and momentum excess characteristic of this class of envelopes around post-AGB stars. Aims. By taking advantage of the new extended configuration of the IRAM Plateau de Bure interferometer, we wanted to study the morphology and velocity field of the molecular gas better in this nebula, particularly in its central part.Methods. We performed sub-arcsecond resolution interferometric observations of the J = 2−1 rotational line of 13 CO in M 1-92. Results. We found that the equatorial component is a thin flat disk, which expands radially with a velocity proportional to the distance to the center. The kinetic age of this equatorial flow is very similar to that of the two lobes. The small widths and velocity dispersion in the gas forming the lobe walls confirm that the acceleration responsible for the nebular shape could not last more than 100-120 yr.Conclusions. The present kinematics of the molecular gas can be explained as the result of a single brief acceleration event, after which the nebula reached an expansion velocity field with axial symmetry. In view of the similarity to other objects, we speculate on the possibility that the whole nebula was formed as a result of a magneto-rotational explosion in a common-envelope system.

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“…The polarimetric properties of the Egg are discussed elsewhere (Sahai et al 1998;Weintraub et al 2000;Ueta et al 2005b). To determine proper motion of the nebulosity over the 5.5 yr time interval defined by these two-epoch observations, we followed the method elucidated by Currie et al (1996) and Morse et al (2001) in their proper-motion measurements of Car. This method is based on the idea that proper motion of any local structure in a nebula due to an expansion can be measured by determining the amount of translational shift of the structure via a cross-correlation analysis.…”

Section: Proper-motion Measurementsmentioning

confidence: 99%

Proper‐Motion Measurements of the Cygnus Egg Nebula

Ueta

Murakawa

Meixner

2006

ApJ

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We present the results of proper-motion measurements of the dust shell structure in the Egg Nebula (AFGL 2688, CRL 2688, V1610 Cyg), based on the archived two-epoch data at 2 m taken with the Hubble Space Telescope. We measured the amount of motion of local structures in the nebula by determining their relative shifts over an interval of 5.5 yr. The dynamical age of the nebula is found to be roughly 350 yr based on the overall Hubble-law-esque motion of the nebula. By adopting the deprojected velocity of 45 km s À1 at the tips of the bipolar lobes, our propermotion measurements indicate that the distance to the Egg Nebula is about 420 pc and that the lobes are inclined at 7N7 with respect to the plane of the sky. The refined distance estimate yields a luminosity of the central star of 3:3 ; 10 3 L , a total shell mass of 1.2 M , and a mass-loss rate (the upper limit) of 3:6 ; 10 À3 M yr À1 . Assuming a 0.6 M central post-AGB stellar mass, the initial mass of the Egg is 1.8 M . Upon analysis, we also discovered that (1) the central star of the Egg Nebula has a proper motion of its own at a rate of 17 mas yr À1 , (2) the tips of the lobes increased their velocity due to shock acceleration, and (3) the apparent bipolar lobes consist of multiple outflows at distinct inclination angles projected onto each other.

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[ITAL]Hubble Space Telescope[/ITAL] Proper-Motion Measurements of the η Carinae Nebula

Cited by 81 publications

References 18 publications

Herschelfar-infrared observations of the Carina Nebula complex

Herschelfar-infrared observations of the Carina Nebula complex

Minkowski's footprint revisited

Proper‐Motion Measurements of the Cygnus Egg Nebula

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