The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

Tan, Q; Gao, Yu; Zhang, Zhi-Yu; Greve, T. R.; Jiang, Xue-Jian; Wilson, C. D.; Yang, C.; Bemis, Ashley; Chung, Aeree; Matsushita, Satoki; Shi, Yong; Ao, Yu‐Fei; Brinks, E.; Currie, Malcolm J.; Davis, Timothy A.; Grijs, Richard de; Ho, Luis C.; Imanishi, Masatoshi; Kohno, Kotaro; Lee, Bumhyun; Parsons, Harriet; Rawlings, Mark G.; Rigopoulou, D.; Rosolowsky, Erik; Bulger, J.; Chen, Hao; Chapman, Scott; Eden, David; Gear, Walter Kieran; Gu, Q. S.; He, Jin; Jiao, Qian; Liu, Dai Zhong; Liu, Li Jie; Li, Xiao Hu; Michałowski, M. J.; Nguyen-Luong, Q.; Qiu, J.; Smith, M.; Violino, Giulio; Wang, Jian Fa; Wang, Jun Feng; Wang, Jun Zhi; Yeh, Sherry; Zhao, Yonghua; Zhu, Meiping

doi:10.3847/1538-4357/aac512

Cited by 41 publications

(58 citation statements)

References 129 publications

(213 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We also include infrared archival imaging data from Spitzer (IRAC 3.6 µm and MIPS 24 µm), and Herschel (PACS 70, 100, and 160 µm). The Nobeyama and Herschel data were convolved to 14-arcsec resolution and regridded to the same pixel scale (see Tan et al 2018 for more details of the processing of the ancillary data). This allowed us to calculate the total infrared luminosity L IR (8-1000 µm) in each pixel using a combination of the 24-, 70-, 100-, and 160-µm luminosities (Galametz et al 2013;Tan et al 2018).…”

Section: Ancillary Datamentioning

confidence: 99%

“…To identify detections of the emission lines used in this work, we adopted the same criteria as Tan et al (2018), i.e., we require that the integrated line intensity to be at least three times the "integrated noise" (SNR > 3). The uncer-1 http://www.iram.fr/IRAMFR/GILDAS/ 2 https://www.eaobservatory.org/jcmt/help/workshops/ tainty, σ I , on the integrated line emission is:…”

Section: Data Reductionmentioning

confidence: 99%

“…For HCN 4-3 and HCO + 4-3 the uncertainty of the binning data points is calculated based on the error from the individual pixels (see Section 3.3). For L IR , the uncertainty is 30 per cent at most (Tan et al 2018). For 3.6 µm, the uncertainty is considered to be ∼ 50 per cent.…”

Section: Radial Profile and Concentration Indexmentioning

confidence: 99%

“…The result presented in this paper is uncertain and only indicative , and we look forward to investigating this method for large samples in future studies at higher resolution. Tan et al (2018) reported the integrated-intensity ratios of R HCN43 and R HCO + 43 in different regions of six galaxies. The ratios lie between approximately 0.003 and 0.1, and they are higher in the centre and lower in outer regions.…”

Section: Radial Profile and Concentration Indexmentioning

confidence: 99%

“…Specifically, how do we interpret the variations observed in the Kennicutt-Schmidt (KS) star-formation (SF) relationship (Kennicutt 1998), and how do the density and temperature of molecular gas relate to the starformation rate (SFR), or the star-formation efficiency (SFE, defined as the SFR per unit gas mass)? Since the pioneering studies of Gao & Solomon (2004a,b), it has been shown that the amount of dense molecular gas is tightly and linearly correlated with the SFR of individual galaxies (in logarithmic scale), where dense gas is usually defined as gas with a volume density n > 10 4 cm −3 , and can be traced by molecular emission lines with high critical densities (n crit ) like E-mail: xjjiang@pmo.ac.cn; x.jiang@eaobservatory.org HCN (Baan et al 2008;Graciá-Carpio et al 2008;Juneau et al 2009;Lada et al 2010;Greve et al 2014;Liu et al 2015b,a;Zhang et al 2014;Chen et al 2015;Braine et al 2017;Tan et al 2018). Meanwhile, observations on smaller scales, such as of resolved galaxy structures or of molecular clouds in the Milky Way, also showed that star-forming sites are mainly associated with dense structures (Wu et al 2005;André et al 2014;Liu et al 2016;Stephens et al 2016;Shimajiri et al 2017).…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

The MALATANG survey: dense gas and star formation from high-transition HCN and HCO+ maps of NGC 253

Jiang

Greve

Gao

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

To study the high-transition dense-gas tracers and their relationships to the star formation of the inner ∼ 2 kpc circumnuclear region of NGC 253, we present HCN J = 4 − 3 and HCO + J = 4 − 3 maps obtained with the James Clerk Maxwell Telescope (JCMT). With the spatially resolved data, we compute the concentration indices r 90 /r 50 for the different tracers. HCN and HCO + 4-3 emission features tend to be centrally concentrated, which is in contrast to the shallower distribution of CO 1-0 and the stellar component. The dense-gas fraction ( f dense , traced by the velocity-integratedintensity ratios of HCN/CO and HCO + /CO) and the ratio R 31 (CO 3-2/1-0) decline towards larger galactocentric distances, but increase with higher SFR surface density. The radial variation and the large scatter of f dense and R 31 imply distinct physical conditions in different regions of the galactic disc. The relationships of f dense versus Σ stellar , and SFE dense versus Σ stellar are explored. SFE dense increases with higher Σ stellar in this galaxy, which is inconsistent with previous work that used HCN 1-0 data. This implies that existing stellar components might have different effects on the high-J HCN and HCO + than their low-J emission. We also find that SFE dense seems to be decreasing with higher f dense which is consistent with previous works, and it suggests that the ability of the dense gas to form stars diminishes when the average density of the gas increases. This is expected in a scenario where only the regions with high-density contrast collapse and form stars.

show abstract

Section: Ancillary Datamentioning

confidence: 99%

Section: Data Reductionmentioning

confidence: 99%

Section: Radial Profile and Concentration Indexmentioning

confidence: 99%

Section: Radial Profile and Concentration Indexmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The MALATANG survey: dense gas and star formation from high-transition HCN and HCO+ maps of NGC 253

Jiang

Greve

Gao

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

A global correlation linking young stars, clouds, and galaxies

Mendigutía

Lada

Oudmaijer

2018

A&A

View full text Add to dashboard Cite

Context. The star formation rate (SFR) linearly correlates with the amount of dense gas mass (M dg ) involved in the formation of stars both for distant galaxies and clouds in our Galaxy. Similarly, the mass accretion rate (Ṁ acc ) and the disk mass (M disk ) of young, Class II stars are also linearly correlated. Aims. We aim to explore the conditions under which the previous relations could be unified. Methods. Observational values of SFR, M dg ,Ṁ acc , and M disk for a representative sample of galaxies, star forming clouds, and young stars have been compiled from the literature. Data were plotted together in order to analyze how the rate of gas transformed into stars and the mass of dense gas directly involved in this transformation relate to each other over vastly different physical systems. Results. A statistically significant correlation is found spanning ∼ 16 orders of magnitude in each axis, but with large scatter. This probably represents one of the widest ranges of any empirical correlation known, encompassing galaxies that are several kiloparsec in size, parsec-size star-forming clouds within our Galaxy, down to young, pre-main sequence stars with astronomical unit-size protoplanetary disks. Assuming that this global correlation has an underlying physical reason, we propose a bottom-up hypothesis suggesting that a relation betweenṀ acc and the total circumstellar mass surrounding Class 0/I sources (M cs ; disk+envelope) drives the correlation in clouds that host protostars and galaxies that host clouds. This hypothesis is consistent with the fact that the SFRs derived for clouds over a timescale of 2 Myr can be roughly recovered from the sum of instantaneous accretion rates of the protostars embedded within them, implying that galactic SFRs averaged over ∼ 10-100 Myr should be constant over this period too. Moreover, the sum of the circumstellar masses directly participating in the formation of the protostellar population in a cloud likely represents a non-negligible fraction of the dense gas mass within the cloud.Conclusions. If the fraction of gas directly participating in the formation of stars is ∼ 1-35% of the dense gas mass associated with star-forming clouds and galaxies, then the global correlation for all scales has a near unity slope and an intercept consistent with the (proto-)stellar accretion timescale, M cs /Ṁ acc . Therefore, an additional critical test of our hypothesis is that theṀ acc -M disk correlation for Class II stars should also be observed betweenṀ acc and M cs for Class 0/I sources with similar slope and intercept.

show abstract

ALMA view of the¹²C/¹³C isotopic ratio in starburst galaxies

Tang

Henkel

Menten

et al. 2019

A&A

View full text Add to dashboard Cite

We derive molecular-gas-phase 12 C/ 13 C isotope ratios for the central few 100 pc of the three nearby starburst galaxies NGC 253, NGC 1068, and NGC 4945 making use of the λ ∼ 3 mm 12 CN and 13 CN N = 1-0 lines in the ALMA Band 3. The 12 C/ 13 C isotopic ratios derived from the ratios of these lines range from 30 to 67 with an average of 41.6 ± 0.2 in NGC 253, from 24 to 62 with an average of 38.3 ± 0.4 in NGC 1068, and from 6 to 44 with an average of 16.9 ± 0.3 in NGC 4945. The highest 12 C/ 13 C isotopic ratios are determined in some of the outskirts of the nuclear regions of the three starburst galaxies. The lowest ratios are associated with the northeastern and southwestern molecular peaks of NGC 253, the northeastern and southwestern edge of the mapped region in NGC 1068, and the very center of NGC 4945. In case of NGC 1068, the measured ratios suggest inflow from the outer part of NGC 1068 into the circum-nuclear disk through both the halo and the bar. Low 12 C/ 13 C isotopic ratios in the central regions of these starburst galaxies indicate the presence of highly processed material.

show abstract

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

Cited by 41 publications

References 129 publications

The MALATANG survey: dense gas and star formation from high-transition HCN and HCO+ maps of NGC 253

The MALATANG survey: dense gas and star formation from high-transition HCN and HCO+ maps of NGC 253

A global correlation linking young stars, clouds, and galaxies

ALMA view of the¹²C/¹³C isotopic ratio in starburst galaxies

Contact Info

Product

Resources

About

The MALATANG Survey: The LGAS–LIR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

Cited by 41 publications

References 129 publications

The MALATANG survey: dense gas and star formation from high-transition HCN and HCO+ maps of NGC 253

The MALATANG survey: dense gas and star formation from high-transition HCN and HCO+ maps of NGC 253

A global correlation linking young stars, clouds, and galaxies

ALMA view of the12C/13C isotopic ratio in starburst galaxies

Contact Info

Product

Resources

About

The MALATANG Survey: The L_GAS–L_IR Correlation on Sub-kiloparsec Scale in Six Nearby Star-forming Galaxies as Traced by HCN J = 4 → 3 and HCO⁺ J = 4 → 3

ALMA view of the¹²C/¹³C isotopic ratio in starburst galaxies