J/ApJ/905/55 Bright-PAH galaxies from AKARI & Spitzer (ASESS) (Lai+, 2020)
All the PAHs: an AKARI-Spitzer cross-archival spectroscopic survey of aromatic
emission in galaxies.
Lai T.S.-Y., Smith J.D.T., Baba S., Spoon H.W.W., Imanishi M.
<Astrophys. J., 905, 55 (2020)>
=2020ApJ...905...55L 2020ApJ...905...55L
ADC_Keywords: Galaxies, IR; Star Forming Region; Interstellar medium;
Equivalent widths; Surveys
Keywords: Polycyclic aromatic hydrocarbons ; Interstellar dust extinction ;
Starburst galaxies ; Luminous infrared galaxies ;
Ultraluminous infrared galaxies
Abstract:
We present a large sample of 2.5-38µm galaxy spectra drawn from a
cross-archival comparison in the AKARI-Spitzer Extragalactic Spectral
Survey, and investigate a subset of 113 star-forming galaxies with
prominent polycyclic aromatic hydrocarbon (PAH) emission spanning a
wide range of star formation properties. With AKARI's extended
2.5-5µm wavelength coverage, we self-consistently model for the
first time all PAH emission bands using a modified version of PAHfit.
We find LPAH3.3/LIR∼0.1%, and the 3.3µm PAH feature contributes
∼1.5%-3% to the total PAH power-somewhat less than earlier dust models
have assumed. We establish a calibration between 3.3µm PAH emission
and star formation rate, but also find regimes where it loses
reliability, including at high luminosity and low metallicity. The
3.4µm aliphatic emission and a broad plateau feature centered at
3.47µm are also modeled. As the PAH feature with the shortest
wavelength, the one at 3.3µm is susceptible to attenuation, leading
to differences of a factor of ∼3 in the inferred star formation rate
at high obscuration with different assumed attenuation geometries.
Surprisingly, LPAH3.3/LΣPAH shows no sign of decline at high
luminosities, and the low-metallicity dwarf galaxy II Zw 40 exhibits
an unusually strong 3.3µm band; both results suggest either that
the smallest PAHs are better able to survive under intense radiation
fields than presumed, or that PAH emission is shifted to shorter
wavelengths in intense and high-energy radiation environments. A
photometric surrogate for 3.3µm PAH luminosity using JWST/NIRCam is
provided and found to be highly reliable at low redshift.
Description:
The AKARI-Spitzer Extragalactic Spectral Survey (ASESS) sample is
drawn from an exhaustive cross-archival comparison between the
Infrared Database of Extragalactic Observables from Spitzer (IDEOS)
catalog (Hernan-Caballero+ 2016, J/MNRAS/455/1796) and the public data
provided by AKARI Infrared Camera (IRC) pointed spectroscopic
observations compiled in the DARTS database provided by ISAS, JAXA.
In this cross-archival comparison, only the AKARI/IRC spectroscopic
observations of 2220 galaxies with higher resolution NG/grism mode
(spectral range from 2.5 to 5um with R∼120 at 3.6um) are considered.
Also considered are 3361 IDEOS galaxies with Spitzer/IRS
low-resolution (R∼60-125) staring-mode observations covering the
spectral range from 5.2 to 38um.
See Section 2.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 69 113 Bright-PAH sample in the AKARI-Spitzer
Extragalactic Spectral Survey (ASESS)
table3.dat 161 113 PAHfit result of bright-PAH sample in
the mixed geometry
table4.dat 161 113 PAHfit result of bright-PAH sample in
the obscured continuum geometry
table6.dat 89 113 Observation for bright-PAH galaxies
fig6.dat 16 10160 Galaxy templates of the eight classes
defined in Figure 1(a)
--------------------------------------------------------------------------------
See also:
VI/64 : Recombination line intensities for hydrogenic ions (Storey+ 1995)
J/AJ/126/1607 : IRAS Revised Bright Galaxy Sample (Sanders+, 2003)
J/ApJ/656/770 : Mid-IR spectrum of star-forming galaxies (Smith+, 2007)
J/ApJ/705/885 : PAH in galaxies at z∼0.1 (O'Dowd+, 2009)
J/MNRAS/405/2505 : Nuclear activity in ULIRGs (Nardini+, 2010)
J/ApJ/723/895 : IR luminosities and aromatic features of 5MUSES (Wu+, 2010)
J/ApJ/744/20 : S4MC project: 6 star forming reg. PAHs (Sandstrom+, 2012)
J/PASJ/65/103 : PAH3.3um/IR luminosity for infrared galaxies (Yamada+, 2013)
J/ApJ/790/124 : Dust and gas physics of the GOALS sample (Stierwalt+, 2014)
J/MNRAS/455/1796 : IDEOS redshift catalogue (Hernan-Caballero+, 2016)
J/MNRAS/469/4933 : Extended red emission in IC59 and IC63 (Lai+, 2017)
J/A+A/617/A130 : Luminous infrared galaxies AKARI 2.5-5um data (Inami+, 2018)
J/ApJ/884/136 : PAH data of star-forming gal. using Spitzer/IRS (Xie+, 2019)
J/ApJ/895/38 : MIR extinction toward Cyg OB2-12 ISM (Hensley+, 2020)
http://darts.isas.jaxa.jp/astro/akari/pointing/ : DARTS database
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 24 A24 --- Name IDEOS galaxy identifier
26 A1 --- n_Name a = also "II Zw 40"
28- 32 F5.3 --- z [0.003/0.191] Spectroscopic redshift
34- 41 F8.4 deg RAdeg [2.47/358] Right Ascension (J2000)
43- 50 F8.4 deg DEdeg [-69.3/81.01] Declination (J2000)
52- 55 F4.2 um EW [0.04/0.92] The 6.2um PAH equivalent width
57- 61 F5.2 --- SSi [-1.4/-0.01] Strength of 9.7um silicate
feature (1)
63- 67 F5.2 [Lsun] logLIR [9.37/12.47]? log 8-1000um IR luminosity (2)
69 A1 --- r_logLIR Reference code for logLIR (3)
--------------------------------------------------------------------------------
Note (1): Defined by the ratio of observed flux intensity (f9.7um) to
continuum flux density (C9.7um) at 9.7um,
SSi=ln(f9.7um/C9.7um).
Note (2): Derived from IRAS fluxes and calculated from
LIR(erg/s)=2.1e39*D(Mpc)2*(13.48*f12+5.16*f25+2.58*f60+f100)
(Sanders & Mirabel 1996ARA&A..34..749S 1996ARA&A..34..749S). For fluxes in IRAS with
upper limits, the prescriptions in Imanishi+ (2008PASJ...60S.489I 2008PASJ...60S.489I &
2010ApJ...721.1233I 2010ApJ...721.1233I) are followed.
Note (3): Reference as follows:
1 = Moshir et al. 1993, Cat. II/156
2 = Sanders et al. 2003, Cat. J/AJ/126/1607
3 = Imanishi et al. 2008PASJ...60S.489I 2008PASJ...60S.489I
4 = Imanishi et al. 2010ApJ...721.1233I 2010ApJ...721.1233I
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table[34].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 24 A24 --- Name IDEOS galaxy identifier
26- 32 F7.3 10+7Lsun L3.3 [0.03/475] Integrated luminosity of 3.3um
emission feature (1)
34- 39 F6.3 10+7Lsun e_L3.3 [0.005/68] Uncertainty in L3.3
41 A1 --- l_L3.4 The 3σ upper limit on L3.4
42- 48 F7.3 10+7Lsun L3.4 [0.012/34]? Integrated luminosity of 3.4um
emission feature (1)
50- 53 F4.2 10+7Lsun e_L3.4 [0.01/4]? Uncertainty in L3.4
55 A1 --- l_L3.47 The 3σ upper limit on L3.47
56- 62 F7.3 10+7Lsun L3.47 [0.012/45]? Integrated luminosity of 3.47um
emission feature (1)
64- 68 F5.3 10+7Lsun e_L3.47 [0.003/6]? Uncertainty in L3.47
70- 76 F7.3 10+8Lsun L6.2 [0.01/108.1] Integrated luminosity of
primary 6.2um PAH emission
78- 82 F5.3 10+8Lsun e_L6.2 [0.001/4] Uncertainty in L6.2
84- 90 F7.3 10+8Lsun L11.3 [0.009/113]? Integrated luminosity of
primary 11.3um complex PAH emission
92- 96 F5.3 10+8Lsun e_L11.3 [0.001/5.2]? Uncertainty in L11.3
98 A1 --- l_L17 The 3σ upper limit on L17
99- 104 F6.2 10+8Lsun L17 [0.18/73.4]? Integrated luminosity of
primary 17um complex PAH emission
106- 109 F4.2 10+8Lsun e_L17 [0.01/10]? Uncertainty in L17
111- 117 F7.3 10+9Lsun Sigma [0.013/112] Total integrated PAH luminosity
119- 123 F5.3 10+9Lsun e_Sigma [0.001/2.2] Uncertainty in Sigma
125- 131 F7.3 10+7Lsun LNeII [0.037/231] Integrated Ne II line emission
133- 138 F6.3 10+7Lsun e_LNeII [0.001/16] Uncertainty in LNeII
140 A1 --- l_LNeIII The 3σ upper limit on LNeIII
141- 147 F7.3 10+7Lsun LNeIII [0.07/253]? Integrated Ne III line emission
149- 154 F6.3 10+7Lsun e_LNeIII [0.0/13]? Uncertainty in NeIIII
156- 161 F6.2 Msun/yr SFR [0.4/377]? Neon line inferred star
formation rate (1)
--------------------------------------------------------------------------------
Note (1): Only provided are galaxies with >3σ detections in
both [NeII] and [NeIII].
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
-------------------------------------------------------------------------------
1- 21 A21 --- ID AKARI/IRC galaxy identifier
23- 46 A24 --- Name IDEOS galaxy identifier
48- 54 I7 --- obsIRC [1100011/5200268] IRC observation identifier
56- 70 A15 --- IRCsID IRC sub-ID identifier
72- 78 A7 --- Phase IRC phase
80- 89 A10 --- ObsID IDEOS observation identifier
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Class Galaxy template class (see Section 2.5)
4- 9 F6.3 um lambda [2.6/28] Wavelength
11- 16 F6.3 --- Flux [0.05/32.1] Density normalized fν at 6.2um
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-May-2022