Erratum: Radio emission from dust-obscured galaxies

Gabányi, Krisztina É; Frey, Sándor; Perger, Krisztina

doi:10.1093/mnras/stab3812

errata, addenda, radio continuum: galaxies, galaxies: star formation, galaxies: active, methods: data analysis

The paper, ’Radio emission from dust-obscured galaxies’ was published in the Monthly Notices of the Royal Astronomical Society, Volume 506, Issue 3, pp. 3641–3647 (2021). After publication, we noticed an error in the calculation of the radio power of the dust-obscured galaxies (DOG) detected in the Faint Images of the Radio Sky at Twenty-Centimeters (FIRST, Helfand, White & Becker 2015) survey, listed in the last column of Table 3 of the original paper. A multiplicative factor of ∼9 originating from a wrong unit conversion was left out, therefore the true radio power values are larger. Additionally, we correct two typos in the luminosity distances for HSC J140638.20 + 010254.6 and SST24 J143644.2 + 350627. We give here the correct version of the original Table 3. As in the original paper, we assume a flat ΛCDM cosmological model with |$H_0=70\, \text{km s}^{-1}\text{Mpc}^{-1}$|⁠, Ω_m = 0.27, and |$\Omega _\Lambda =0.73$|⁠. The 1.4-GHz radio power was calculated as

$$\begin{eqnarray*} P_{1.4\text{GHz}}=4\pi D^2_\text{L}S_\text{int} (1+z)^{(-\alpha -1)}, \end{eqnarray*}$$

(1)

where D_L is the luminosity distance, z is the redshift, S_int is the integrated 1.4-GHz flux density, and α is the spectral index. The spectral index is defined as S ∼ ν^α, where ν is the observing frequency. Here like in the original paper, we assumed α = 0.

Accordingly, the star formation rates estimated from the 1.4-GHz radio powers using the formula of Hopkins et al. (2003) are also approximately an order of magnitude higher, and thus only the one FIRST-detected bump DOG has a star formation rate less than |$100 \mathrm{\, M}_\odot \mathrm{\, yr}^{-1}$| (even the faintest power-law DOG, HSC J140738.47 + 002731.4 has a star formation rate exceeding this value). Consequently, the highest star formation rate exceeds |$10^5 \mathrm{\, M}_\odot \mathrm{\, yr}^{-1}$|⁠. This correction makes the original conclusion that radio-emitting AGN may contribute to the radio emission in at least part of the FIRST-detected DOG sources even stronger.

Table 3.

Open in new tab

Details of the FIRST-detected DOGs. In the upper part, the FIRST-detected sources from Noboriguchi et al. (2019) are listed, here only photometric redshifts (z_ph) are available. In the lower part, the FIRST-detected sources from Bussmann et al. (2012) and Melbourne et al. (2012) are listed, they have spectroscopic redshifts. The name and classification of each source is given in columns 1 and 2, respectively. The redshift (either photometric or spectroscopic), and the luminosity distance (D_L) is given in columns 3 and 4, respectively. We list the sidelobe probability, peak intensity, integrated flux density, and rms noise level (all from the FIRST catalog of Helfand et al. 2015) in columns 5, 6, 7, and 8, respectively. In the last two columns, the compactness parameter (i.e. the ratio of the peak intensity to the integrated flux density) and the 1.4-GHz radio power are given.

ID	Class	z_ph / z	D_L	p_s	S_peak	S_int	rms	Comp.	P_1.4GHz
			Mpc		mJy beam⁻¹	mJy	mJy		10²² W Hz⁻¹
HSC J083713.56 + 021707.1	PL	1.05	7151.9	0.014	1.23	1.02	0.141	1.21	305
HSC J085552.54 + 014553.2	PL	1.50	11161.1	0.014	2.44	2.07	0.154	1.18	1234
HSC J091128.32 − 011812.2	PL	1.53	11445	0.014	70.32	72.62	0.145	0.97	44986
HSC J091218.78 − 000401.3	PL	1.38	10063.1	0.014	17.89	19.30	0.14	0.93	9826
HSC J091854.50 + 015046.6*	PL	1.12	7752.6	0.528	1.13	1.14	0.152	0.99	387
HSC J140256.23 − 000347.7	PL	1.55	11631.7	0.058	1.15	0.81	0.133	1.42	514
HSC J140444.81 + 002451.1	B	0.05	222.5	0.014	10.95	11.44	0.151	0.96	6.5
HSC J140638.20 + 010254.6	PL	0.236^a	1186.6	0.014	8.24	9.19	0.154	0.90	125
HSC J140738.47 + 002731.4	PL	0.54	3142.9	0.014	1.55	0.89	0.15	1.74	68
HSC J141546.89 − 011451.7*	PL	1.06	7237.1	0.452	1.05	3.01	0.154	0.35	916
HSC J141955.59 − 003449.1	PL	1.95	15466.4	0.014	16.89	17.48	0.145	0.97	16959
HSC J142207.90 − 002408.5	U	0.99	6645.2	0.014	4.11	3.62	0.152	1.13	961
HSC J142332.74 − 012526.8	U	0.52	3002.2	0.014	1.45	1.66	0.15	0.87	118
HSC J142435.43 + 005947.8*	PL	1.22	8627.3	0.188	1.19	1.34	0.155	0.89	538
HSC J143004.57 + 011653.4	U	0.86	5575.6	0.014	2.85	2.90	0.137	0.98	580
HSC J144557.52 − 002847.0	PL	–	–	0.014	2.92	2.81	0.172	1.04	–
HSC J144740.41 − 013524.0	PL	0.98	6561.5	0.014	1.35	1.78	0.146	0.76	463
HSC J144814.45 + 005302.3	PL	0.98	6561.5	0.098	1.11	0.71	0.14	1.56	185
HSC J145753.79 + 000508.5	PL	1.12	7752.6	0.014	1.94	1.93	0.152	1.00	655
SST24 J142648.9 + 332927	PL	2.00	15957.9	0.014	1.63	1.42	0.142	1.15	1442
SST24 J142842.9 + 342409	PL	2.18	17746.6	0.039	1.25	1.29	0.132	0.97	1529
SST24 J143102.2 + 325152	PL	2.00	15957.9	0.014	2.10	1.57	0.116	1.34	1595
SST J143430.6 + 342757	PL	1.24	8804.4	0.014	1.37	1.49	0.134	0.92	617
SST J143541.2 + 334228	PL	1.39	10154.2	0.014	1.26	1.46	0.13	0.86	754
SST24 J143644.2 + 350627	PL	1.95^b	15466.4	0.014	4.25	4.81	0.142	0.88	4667

ID	Class	z_ph / z	D_L	p_s	S_peak	S_int	rms	Comp.	P_1.4GHz
			Mpc		mJy beam⁻¹	mJy	mJy		10²² W Hz⁻¹
HSC J083713.56 + 021707.1	PL	1.05	7151.9	0.014	1.23	1.02	0.141	1.21	305
HSC J085552.54 + 014553.2	PL	1.50	11161.1	0.014	2.44	2.07	0.154	1.18	1234
HSC J091128.32 − 011812.2	PL	1.53	11445	0.014	70.32	72.62	0.145	0.97	44986
HSC J091218.78 − 000401.3	PL	1.38	10063.1	0.014	17.89	19.30	0.14	0.93	9826
HSC J091854.50 + 015046.6*	PL	1.12	7752.6	0.528	1.13	1.14	0.152	0.99	387
HSC J140256.23 − 000347.7	PL	1.55	11631.7	0.058	1.15	0.81	0.133	1.42	514
HSC J140444.81 + 002451.1	B	0.05	222.5	0.014	10.95	11.44	0.151	0.96	6.5
HSC J140638.20 + 010254.6	PL	0.236^a	1186.6	0.014	8.24	9.19	0.154	0.90	125
HSC J140738.47 + 002731.4	PL	0.54	3142.9	0.014	1.55	0.89	0.15	1.74	68
HSC J141546.89 − 011451.7*	PL	1.06	7237.1	0.452	1.05	3.01	0.154	0.35	916
HSC J141955.59 − 003449.1	PL	1.95	15466.4	0.014	16.89	17.48	0.145	0.97	16959
HSC J142207.90 − 002408.5	U	0.99	6645.2	0.014	4.11	3.62	0.152	1.13	961
HSC J142332.74 − 012526.8	U	0.52	3002.2	0.014	1.45	1.66	0.15	0.87	118
HSC J142435.43 + 005947.8*	PL	1.22	8627.3	0.188	1.19	1.34	0.155	0.89	538
HSC J143004.57 + 011653.4	U	0.86	5575.6	0.014	2.85	2.90	0.137	0.98	580
HSC J144557.52 − 002847.0	PL	–	–	0.014	2.92	2.81	0.172	1.04	–
HSC J144740.41 − 013524.0	PL	0.98	6561.5	0.014	1.35	1.78	0.146	0.76	463
HSC J144814.45 + 005302.3	PL	0.98	6561.5	0.098	1.11	0.71	0.14	1.56	185
HSC J145753.79 + 000508.5	PL	1.12	7752.6	0.014	1.94	1.93	0.152	1.00	655
SST24 J142648.9 + 332927	PL	2.00	15957.9	0.014	1.63	1.42	0.142	1.15	1442
SST24 J142842.9 + 342409	PL	2.18	17746.6	0.039	1.25	1.29	0.132	0.97	1529
SST24 J143102.2 + 325152	PL	2.00	15957.9	0.014	2.10	1.57	0.116	1.34	1595
SST J143430.6 + 342757	PL	1.24	8804.4	0.014	1.37	1.49	0.134	0.92	617
SST J143541.2 + 334228	PL	1.39	10154.2	0.014	1.26	1.46	0.13	0.86	754
SST24 J143644.2 + 350627	PL	1.95^b	15466.4	0.014	4.25	4.81	0.142	0.88	4667

Notes. *The FIRST source can be a spurious detection caused by sidelobes of unrelated bright sources.

a

The used value is spectroscopic redshift from SDSS DR9 (Ahn et al. 2012). Noboriguchi et al. (2019) used z_ph = 0.68.

b

A slightly different spectroscopic redshift, z = 1.84 is given by Hernán-Caballero et al. (2016).

Table 3.

Open in new tab

Details of the FIRST-detected DOGs. In the upper part, the FIRST-detected sources from Noboriguchi et al. (2019) are listed, here only photometric redshifts (z_ph) are available. In the lower part, the FIRST-detected sources from Bussmann et al. (2012) and Melbourne et al. (2012) are listed, they have spectroscopic redshifts. The name and classification of each source is given in columns 1 and 2, respectively. The redshift (either photometric or spectroscopic), and the luminosity distance (D_L) is given in columns 3 and 4, respectively. We list the sidelobe probability, peak intensity, integrated flux density, and rms noise level (all from the FIRST catalog of Helfand et al. 2015) in columns 5, 6, 7, and 8, respectively. In the last two columns, the compactness parameter (i.e. the ratio of the peak intensity to the integrated flux density) and the 1.4-GHz radio power are given.

ID	Class	z_ph / z	D_L	p_s	S_peak	S_int	rms	Comp.	P_1.4GHz
			Mpc		mJy beam⁻¹	mJy	mJy		10²² W Hz⁻¹
HSC J083713.56 + 021707.1	PL	1.05	7151.9	0.014	1.23	1.02	0.141	1.21	305
HSC J085552.54 + 014553.2	PL	1.50	11161.1	0.014	2.44	2.07	0.154	1.18	1234
HSC J091128.32 − 011812.2	PL	1.53	11445	0.014	70.32	72.62	0.145	0.97	44986
HSC J091218.78 − 000401.3	PL	1.38	10063.1	0.014	17.89	19.30	0.14	0.93	9826
HSC J091854.50 + 015046.6*	PL	1.12	7752.6	0.528	1.13	1.14	0.152	0.99	387
HSC J140256.23 − 000347.7	PL	1.55	11631.7	0.058	1.15	0.81	0.133	1.42	514
HSC J140444.81 + 002451.1	B	0.05	222.5	0.014	10.95	11.44	0.151	0.96	6.5
HSC J140638.20 + 010254.6	PL	0.236^a	1186.6	0.014	8.24	9.19	0.154	0.90	125
HSC J140738.47 + 002731.4	PL	0.54	3142.9	0.014	1.55	0.89	0.15	1.74	68
HSC J141546.89 − 011451.7*	PL	1.06	7237.1	0.452	1.05	3.01	0.154	0.35	916
HSC J141955.59 − 003449.1	PL	1.95	15466.4	0.014	16.89	17.48	0.145	0.97	16959
HSC J142207.90 − 002408.5	U	0.99	6645.2	0.014	4.11	3.62	0.152	1.13	961
HSC J142332.74 − 012526.8	U	0.52	3002.2	0.014	1.45	1.66	0.15	0.87	118
HSC J142435.43 + 005947.8*	PL	1.22	8627.3	0.188	1.19	1.34	0.155	0.89	538
HSC J143004.57 + 011653.4	U	0.86	5575.6	0.014	2.85	2.90	0.137	0.98	580
HSC J144557.52 − 002847.0	PL	–	–	0.014	2.92	2.81	0.172	1.04	–
HSC J144740.41 − 013524.0	PL	0.98	6561.5	0.014	1.35	1.78	0.146	0.76	463
HSC J144814.45 + 005302.3	PL	0.98	6561.5	0.098	1.11	0.71	0.14	1.56	185
HSC J145753.79 + 000508.5	PL	1.12	7752.6	0.014	1.94	1.93	0.152	1.00	655
SST24 J142648.9 + 332927	PL	2.00	15957.9	0.014	1.63	1.42	0.142	1.15	1442
SST24 J142842.9 + 342409	PL	2.18	17746.6	0.039	1.25	1.29	0.132	0.97	1529
SST24 J143102.2 + 325152	PL	2.00	15957.9	0.014	2.10	1.57	0.116	1.34	1595
SST J143430.6 + 342757	PL	1.24	8804.4	0.014	1.37	1.49	0.134	0.92	617
SST J143541.2 + 334228	PL	1.39	10154.2	0.014	1.26	1.46	0.13	0.86	754
SST24 J143644.2 + 350627	PL	1.95^b	15466.4	0.014	4.25	4.81	0.142	0.88	4667

ID	Class	z_ph / z	D_L	p_s	S_peak	S_int	rms	Comp.	P_1.4GHz
			Mpc		mJy beam⁻¹	mJy	mJy		10²² W Hz⁻¹
HSC J083713.56 + 021707.1	PL	1.05	7151.9	0.014	1.23	1.02	0.141	1.21	305
HSC J085552.54 + 014553.2	PL	1.50	11161.1	0.014	2.44	2.07	0.154	1.18	1234
HSC J091128.32 − 011812.2	PL	1.53	11445	0.014	70.32	72.62	0.145	0.97	44986
HSC J091218.78 − 000401.3	PL	1.38	10063.1	0.014	17.89	19.30	0.14	0.93	9826
HSC J091854.50 + 015046.6*	PL	1.12	7752.6	0.528	1.13	1.14	0.152	0.99	387
HSC J140256.23 − 000347.7	PL	1.55	11631.7	0.058	1.15	0.81	0.133	1.42	514
HSC J140444.81 + 002451.1	B	0.05	222.5	0.014	10.95	11.44	0.151	0.96	6.5
HSC J140638.20 + 010254.6	PL	0.236^a	1186.6	0.014	8.24	9.19	0.154	0.90	125
HSC J140738.47 + 002731.4	PL	0.54	3142.9	0.014	1.55	0.89	0.15	1.74	68
HSC J141546.89 − 011451.7*	PL	1.06	7237.1	0.452	1.05	3.01	0.154	0.35	916
HSC J141955.59 − 003449.1	PL	1.95	15466.4	0.014	16.89	17.48	0.145	0.97	16959
HSC J142207.90 − 002408.5	U	0.99	6645.2	0.014	4.11	3.62	0.152	1.13	961
HSC J142332.74 − 012526.8	U	0.52	3002.2	0.014	1.45	1.66	0.15	0.87	118
HSC J142435.43 + 005947.8*	PL	1.22	8627.3	0.188	1.19	1.34	0.155	0.89	538
HSC J143004.57 + 011653.4	U	0.86	5575.6	0.014	2.85	2.90	0.137	0.98	580
HSC J144557.52 − 002847.0	PL	–	–	0.014	2.92	2.81	0.172	1.04	–
HSC J144740.41 − 013524.0	PL	0.98	6561.5	0.014	1.35	1.78	0.146	0.76	463
HSC J144814.45 + 005302.3	PL	0.98	6561.5	0.098	1.11	0.71	0.14	1.56	185
HSC J145753.79 + 000508.5	PL	1.12	7752.6	0.014	1.94	1.93	0.152	1.00	655
SST24 J142648.9 + 332927	PL	2.00	15957.9	0.014	1.63	1.42	0.142	1.15	1442
SST24 J142842.9 + 342409	PL	2.18	17746.6	0.039	1.25	1.29	0.132	0.97	1529
SST24 J143102.2 + 325152	PL	2.00	15957.9	0.014	2.10	1.57	0.116	1.34	1595
SST J143430.6 + 342757	PL	1.24	8804.4	0.014	1.37	1.49	0.134	0.92	617
SST J143541.2 + 334228	PL	1.39	10154.2	0.014	1.26	1.46	0.13	0.86	754
SST24 J143644.2 + 350627	PL	1.95^b	15466.4	0.014	4.25	4.81	0.142	0.88	4667

Notes. *The FIRST source can be a spurious detection caused by sidelobes of unrelated bright sources.

a

The used value is spectroscopic redshift from SDSS DR9 (Ahn et al. 2012). Noboriguchi et al. (2019) used z_ph = 0.68.

b

A slightly different spectroscopic redshift, z = 1.84 is given by Hernán-Caballero et al. (2016).

DATA AVAILABILITY

The datasets underlying this article were derived from sources in the public domain: FIRST survey database, http://sundog.stsci.edu/.

REFERENCES

Ahn

C. P.

et al. ,

2012

,

ApJS

,

203

,

21

10.1088/0067-0049/203/2/21

Crossref

Search ADS

Bussmann

R. S.

et al. ,

2012

,

ApJ

,

744

,

150

10.1088/0004-637X/744/2/150

Crossref

Search ADS

Helfand

D. J.

,

White

R. L.

,

Becker

R. H.

,

2015

,

ApJ

,

801

,

26

10.1088/0004-637X/801/1/26

Crossref

Search ADS

Hernán-Caballero

A.

,

Spoon

H. W. W.

,

Lebouteiller

V.

,

Rupke

D. S. N.

,

Barry

D. P.

,

2016

,

MNRAS

,

455

,

1796

10.1093/mnras/stv2464

Crossref

Search ADS

Hopkins

A. M.

et al. ,

2003

,

ApJ

,

599

,

971

10.1086/379608

Crossref

Search ADS

Melbourne

J.

et al. ,

2012

,

AJ

,

143

,

125

10.1088/0004-6256/143/5/125

Crossref

Search ADS

Noboriguchi

A.

et al. ,

2019

,

ApJ

,

876

,

132

10.3847/1538-4357/ab1754

Crossref

Search ADS

This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://dbpia.nl.go.kr/journals/pages/open_access/funder_policies/chorus/standard_publication_model)

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Erratum: Radio emission from dust-obscured galaxies

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