CO emission from Centaurus A

Phillips, T. G.; Ellison, Brian N.; Keene, J.; Leighton, Robert B.; Howard, Robert; Masson, C. R.; Sanders, D. B.; Veidt, B.; Young, Kaisa E.

doi:10.1086/185039

Cited by 38 publications

(26 citation statements)

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“…In the Hα data, this splitting was remarked only near the endpoints of our strips (Nicholson et al 1992) most likely because it was not resolved spectroscopically at smaller radii where the velocity separation is smaller. Previous CO observations by Phillips et al (1987) also showed this splitting only at the extremities of these strips, at least partly because of low spatial resolution. The existence of this splitting over the innermost regions has interesting ramifications for the inferred kpc-scale behaviour of the dust lane.…”

Section: Observational Resultsmentioning

confidence: 76%

“…On kpc scales in the dust lane, H I (van Gorkom et al 1990), CO (Phillips et al 1987;Quillen et al 1992) and Hα (Bland et al 1987;Nicholson et al 1992) all partake of the same behaviour and can be used in concert to construct more robust models. For instance, Eckart et al (1999) recently showed that the Hα model of Nicholson et al (1992) can be extended to explain the (mostly red-shifted) atomic and molecular absorption (Israel et al 1990(Israel et al , 1991Wiklind & Combes 1997) as arising in high-altitude gas in the outlying dust lane.…”

Section: Introductionmentioning

confidence: 99%

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CO J = 3-2 mapping of the molecular circumnuclear disk in Centaurus A

Liszt

2001

A&A

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Section: Observational Resultsmentioning

confidence: 76%

Section: Introductionmentioning

confidence: 99%

CO J = 3-2 mapping of the molecular circumnuclear disk in Centaurus A

Liszt

2001

A&A

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“…The molecular hydrogen mass has been calculated in a region of (∼1.5 kpc) diameter to be ∼2 × 10 8 ⊙ by adopting the distance = 3.8 Mpc. By comparing the data with the single dish [28] value of 1 × 10 9 ⊙ (with = 7 Mpc), a difference of 33% is found by using the same distance. This difference is attributed to missing flux, because this data does not contain short spacing information (ACA and single dish), in addition the relatively short observation time and the high uncertainties in data calibration for the mentioned single dish may also participate in increasing the missing flux.…”

Section: Molecular Gas Mass and Surfacementioning

confidence: 97%

“…NGC 5128 shows considerably clear dust lanes that are probably caused by merger activities in the past (see [26,27]). The molecular interstellar medium in the dust lane has been widely studied [28][29][30][31][32][33][34][35][36]. In addition, due to it being a strong source of radio and far infrared and X-ray emissions, it has been investigated in detail over a wide part of observable spectrum [37].…”

Section: Introductionmentioning

confidence: 99%

Star Formation Law at Sub-kpc Scale in the Elliptical Galaxy Centaurus A as Seen by ALMA

Azeez

Abidin

Hwang

et al. 2017

Advances in Astronomy

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We present an extensive analysis of the relationship between star formation rate surface density (∑ SFR) and molecular gas surface density (∑ H 2 ) at sub-kpc scale in the elliptical galaxy Centaurus A (also known as NGC 5128) at the distance 3.8 Mpc.12 CO ( = 2-1) data from Atacama Large Millimetre/Sub-Millimetre Array SV data with very high resolution (2.9 , 0.84 ), as well as 24 m data from the Spitzer Space Telescope, were used. This is one of the first studies of the SF law on Centaurus A at this very high spatial resolution. The results showed a breakdown in star formation law with a 0.49 ± 0.05 index relating ∑ SFR and ∑ H 2 at 185 pc. A significant correlation exists between surface densities of molecular gas and SFR with very long depletion time (68 Gy). In addition we examined the spatially resolved relationship between velocity dispersion and star formation rate surface density for the outer disk of this galaxy and we found that the average velocity dispersion is equal to 11.78 km/s. The velocity dispersion of the molecular ISM for the outer disk is found to follow a power relation with the star formation rate surface density ∝ (∑ SFR) , where is the slope from the ordinary least square fitting. The value of is about 1/ ≈ 2.16 ± 0.40 and is the power law index of the star formation law.

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“…Star formation appears to be a component of the activity occurring in the host galaxies of AGNs-a growing number of radio galaxies and QSOs have detectable amounts of molecular gas and young UV-luminous knots indicative of recent star formation (Phillips et al 1987;Sanders et al 1988a;Lazareff et al 1989;Mirabel et al 1989;Mazzarella et al 1993, hereafter Paper I; Reuter et al 1993;Evans et al 2001;Allen et al 2002;Scoville et al 2003). In addition, the fraction of classical AGNs with dust in their host galaxies is substantial (e.g., Golombek et al 1988;Sanders et al 1989), with $50% of 3C radio galaxies and $70% of Palomar-Green (PG; Schmidt & Green 1983) QSOs at z P 0:12 having IRAS 8 detections at 60 m. The Infrared Space Observatory (ISO) detected thermal dust emission in a larger fraction of radio galaxies and QSOs (Meisenheimer et al 2001;Haas et al 2003Haas et al , 2004, providing further proof of rich ISMs in the host galaxies of radio galaxies and QSOs.…”

Section: Introductionmentioning

confidence: 99%

Untitled

2005

ASTROPHYS J SUPPL S

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This paper reports the latest results from a millimeter-wave (CO) spectroscopic survey of IRAS-detected radio galaxies with L 1:4 GHz $ 10 23 10 28 W Hz À1 in the redshift range z $ 0:02 0:15. The IRAS flux-limited sample contains 33 radio galaxies with different radio morphologies and a broad range of infrared luminosities (L IR ¼ 10 9 10 12 L ), allowing for an investigation of (1) whether low-z radio-selected active galactic nuclei (AGNs) reside in molecular gas-rich host galaxies and (2) whether the CO properties are correlated with the properties of the host galaxy or the AGN. All of the radio galaxies in Mazzarella et al. and Mirabel et al. have been reobserved. Three new CO detections have been made, raising the total number of CO detections to nine and setting the survey detection rate at $25%. Many of the CO lines have double-peaked profiles, and the CO line widths are broad (average Áv FWHM $ 500 AE 130 km s À1 ), exceeding the average CO widths of both ultraluminous infrared galaxies (300 AE 90 km s À1 ) and Palomar-Green QSOs (260 AE 160 km s À1 ), and thus being indicative of massive host galaxies. The CO luminosities translate into molecular gas masses of $(0:4 7) ; 10 9 M , however, the 3 CO upper limits for nondetections do not rule out a molecular gas mass as high as that of the Milky Way ($3 ; 10 9 M ). Optical images of eight out of nine molecular gas-rich radio galaxies show evidence of close companions and/or tidal features. Finally, there is no obvious correlation between radio power and molecular gas mass. However, it is notable that only one F-R II galaxy out of 12 is detected in this CO survey; the remaining detections are of galaxies hosting F-R I and compact radio jets.

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CO emission from Centaurus A

Cited by 38 publications

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CO J = 3-2 mapping of the molecular circumnuclear disk in Centaurus A

CO J = 3-2 mapping of the molecular circumnuclear disk in Centaurus A

Star Formation Law at Sub-kpc Scale in the Elliptical Galaxy Centaurus A as Seen by ALMA

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