Note on the Mass of M92.

Schwarzschild, M.; Bernstein, Susan David

doi:10.1086/146074

Cited by 11 publications

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“…We chose a bin width of 10 ′′ as it provides seven bins, which is a good compromise between having too few bins and having too few sources per bin. Using equation 1 of Schwarzschild & Bernstein (1955), we obtain r = 44.3 ′′ , or 0.28 pc, yielding a dynamical mass estimate of 410 ±260 M ⊙ . By comparison, the gas mass of NGC 6334 I(N) plus SM2 based on single-dish submillimeter continuum observations is 280 M ⊙ , assuming a uniform dust temperature of 30 K (Sandell 2000), after scaling to the new distance of 1.3 kpc.…”

Section: Dynamical Mass and Relaxation Timementioning

confidence: 88%

“…The filled points are the six sources for which we were able to measure the LSR velocity (Table 7). The horizontal dashed lines demarcate the seven 10 wide strips in which the protostars were counted (from north to south: 1, 2, 6, 9, 3, 3, 1) in order to compute the effective distance to be used in the calculation of the dynamical mass in Section 4.3 by the method of Schwarzschild & Bernstein (1955). minimal spanning tree (MST) formed from these 25 sources, as shown in Figure 10.…”

Section: Protocluster Structure and Statisticsmentioning

confidence: 99%

“…Assuming a random orientation of space velocities, the mean square three-dimensional (3D) velocity is then v 2 3D = 3 v 2 1D = 6.15 ± 3.87 km 2 s −2 . The proper effective distance to use in the virial theorem,r, can be determined by numerical integration of the observed strip counts (Schwarzschild & Bernstein 1955). In this case, the strip counts are the number of stars in each horizontal bin shown in Figure 10.…”

Section: Dynamical Mass and Relaxation Timementioning

confidence: 99%

“…We chose a bin width of 10 as it provides seven bins, which is a good compromise between having too few bins and having too few sources per bin. Using Equation (1) of Schwarzschild & Bernstein (1955), we obtainr = 44. 3, or 0.28 pc, yielding a dynamical mass estimate of 410 ± 260 M .…”

Section: Dynamical Mass and Relaxation Timementioning

confidence: 99%

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Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Hunter

Brogan

Cyganowski

et al. 2014

ApJ

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Using the Submillimeter Array (SMA) and Karl G. Jansky Very Large Array, we have imaged the massive protocluster NGC 6334 I(N) at high angular resolution (0. 5 ∼ 650 AU) from 6 cm to 0.87 mm, detecting 18 new compact continuum sources. Three of the new sources are coincident with previously identified H 2 O masers. Together with the previously known sources, these data bring the number of likely protocluster members to 25 for a protostellar density of ∼700 pc −3 . Our preliminary measurement of the Q-parameter of the minimum spanning tree is 0.82-close to the value for a uniform volume distribution. All of the (nine) sources with detections at multiple frequencies have spectral energy distributions consistent with dust emission, and two (SMA 1b and SMA 4) also have long wavelength emission consistent with a central hypercompact H ii region. Thermal spectral line emission, including CH 3 CN, is detected in six sources: LTE model fitting of CH 3 CN (J = 12-11) yields temperatures of 72-373 K, confirming the presence of multiple hot cores. The fitted LSR velocities range from −3.3 to −7.0 km s −1 , with an unbiased mean square deviation of 2.05 km s −1 , implying a protocluster dynamical mass of 410 ± 260 M . From analysis of a wide range of hot core molecules, the kinematics of SMA 1b are consistent with a rotating, infalling Keplerian disk of diameter 800 AU and enclosed mass of 10-30 M that is perpendicular (within 1• ) to the large-scale bipolar outflow axis. A companion to SMA 1b at a projected separation of 0. 45 (590 AU; SMA 1d), which shows no evidence of spectral line emission, is also confirmed. Finally, we detect one 218.4400 GHz and several 229.7588 GHz Class-I CH 3 OH masers.

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Section: Dynamical Mass and Relaxation Timementioning

confidence: 88%

Section: Protocluster Structure and Statisticsmentioning

confidence: 99%

Section: Dynamical Mass and Relaxation Timementioning

confidence: 99%

Section: Dynamical Mass and Relaxation Timementioning

confidence: 99%

See 2 more Smart Citations

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Hunter

Brogan

Cyganowski

et al. 2014

ApJ

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“…Included in Figure 2 are four globular clusters: 47 Tucanae (Feast and Thackeray 1960), M3 (Oort and van Herk 1959;Sandage 1957), M15 (King 1962), and M92 (Schwarzschild and Bernstein 1955;Wilson and Coffeen 1954). Magnitudes and distances were taken from Hogg (1959).…”

Section: Introductionmentioning

confidence: 99%

The Mean Ratio of Mass to the Three-Halves Power of Luminosity for Elliptical and Lenticular Galaxies

Noonan¹

1971

PASP

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The available data on masses of ellipticals and lenticulars are summarized with emphasis on the uncertainties in the ratio R of mass to 10 _0 -6M , where M is the absolute magnitude. With correction for galactic absorption the result is R= 0.30(and, as a by-product, a mean mass-luminosity ratio of 38^^) based on the magnitude scale in the de Vaucouleurs' catalog. The mass-luminosity relations by Poveda, Rood, and Vorontsov-Velyaminov give values of R in the same range. Implications for the mean cosmic density are discussed.

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Über die spektrale Intensitätsverteilun und die Leuchtkraftverteilung von Sternsystemen

Lamla¹

1959

Astron Nachr

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Mittcilungcn d e s A s t r o p h y s i k a l i s c h e n O b s c r v a t o r i u m s P o t s d a m Nr. 74) Von E. LAMLA, Potsdam Mit 13 Abbildungen. (Eingegangcn rgj8 Scptembcr 23)Mit Hilfe der aus vorliegenden Spektralphotometricn gewonneneii Standard-lntensitatsvertcilungen von Einzelsternen vcrschiedener Spektraltypen und Lcuchtkraftgruppen wcrdcn die lntcnsitatsvcrteilungcn von Sternsystemen -Kugelhaufen und elliptischc Nebel .k r e c h n c t und rnit den vorlicgcndcn lkobachtungcn vergliclien. Die erforderlichen Leuchtkraftvertcilungen (LKV) wcrden am Extrapolationen der aiis dcr Beobachtung bckannten LKV dcr licllsten Sterne dcr Kugelhaufen (Population 11) untcr der Jkdingung gcwonnen. daO rnit den LK\' die bcobachteten Uaten uber Gesamtmasse und Gcsarntlcuchtkraft dicscr Systcnie durch die Rcchniing gut wicdergegcbcn wcrdcn konnen. Zur Ermittlung dcr LlCV der E-Scbcl mu0 eine Annahrnc iiber die Form dcr l;arbenhclligkeitsdiagra,nme gcmacht werden.Es gelingt, die Intcnsitatsvertcilungen der E-Ncbcl init LKV zu ermittcln. die sowohl dcr reinen Population 11 als auch der ..altcn" Population I cntspreclren. Insbesondere tritt in dcr rnit Sternen der Population I bcrechnctcn Intensititsverteilung cin Balincrsprung auf, der bci Annahme der reinen Population I1 nicht zii erwartcn ist. Dadurch ist u. IJ. die Moglichkcit gegekn, auf Grund des Intcnsitatsverlaufes irn U V cntscheiden zii kbnnen, zu wclcher Population die Sterne eines E-Nebels LU zahlen sind. Neben der Darstellung dcr beobachteten Intcnsitftsverliufc durch die Hechiiung wcrden auLh die andcren integralen Zustandsparamctcr der Stcrnsystcmc bestimmt. Entsprechcndc Hcchnungen sind fur das lokalc System dcr Sterne der nahercn Sonncnumgebiing durchgcfuhrt wordcn. I. EinleitungUbcr die spektralcn Intcnsitatsvertcilungen des verschmiei ten Kontinuums cxtragalaktisclier Nebel Z(1) sind bis vor wenigen Jahren kcine genaueren quantitativcn Daten bekannt gcwescn, so daB nian versucht hatte, h e I().) dcr Sternsysteme in crstcr Xiherung durch PLAh-cKschc Strahlungskurven darzustellen ([I] und [z]). Dcmgcgeniiber war bekannt, daB zwischcn den Intensitatsverteilungen des verschmicrten Kontinuums dcr Sternsystemc und dcrjcnigen von Einzelsternen bestimmtc charaktcristische Unterschicde vorhandcn sind (siehe [3j bis [5]). Erst J. STERRINS und A. E. WHITFOHD [6! waren 1948 im Rahmen ihrer 6-Farbenphotometrie in der Lagc, zahlenmallige Angabcn iiber die I(;.) verschiedencr cxtragalaktischer Nebel und auch von Kugelhaufen des eigenen galaktischen Systems zii machen. Diese Bcobachtungscrgcbnisse sind relativ auf die spektrale Intensitatsverteilung des Mittels mehrcrer dCo-Sterne bezogengcmesscn im gleichenFarbsystem-, so daB die Daten ohne groDere Schwierigkeitcn auf das System dcr in [7] crmittcltcn absoluten spektralcn lntensitatsverteilungen a().) dcr Einzelsterne verschiedencr Spcktraltypen und 1-cuchtkraftgruppenabsolut bis auf eine unbestimmt bleibcnde Konstante in den absoluten Hclligkeitcn -umgerechnct werden konncn. Hierbei mull eine grollere Unsichcrheit in dc...

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Note on the Mass of M92.

Cited by 11 publications

References 0 publications

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

The Mean Ratio of Mass to the Three-Halves Power of Luminosity for Elliptical and Lenticular Galaxies

Über die spektrale Intensitätsverteilun und die Leuchtkraftverteilung von Sternsystemen

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