New Detections of Galactic Molecular Absorption Systems toward ALMA Calibrator Sources

New Detections of Galactic Molecular Absorption Systems toward ALMA Calibrator Sources

Ryo Ando    11affiliation: Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan Kotaro Kohno    11affiliation: Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan Yoichi Tamura    11affiliation: Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan Takuma Izumi    11affiliation: Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan Hideki Umehata    11affiliation: Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan 22affiliation: European Southern Observatory, Karl Schwarzschild Str. 2, D-85748 Garching, Germany and Hiroshi Nagai33affiliation: National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

We report on Atacama Large Millimeter/submillimeter Array (ALMA) detections of molecular absorption lines in Bands 3, 6 and 7 toward four radio-loud quasars, which were observed as the bandpass and complex gain calibrators. The absorption systems, three of which are newly detected, are found to be Galactic origin. Moreover, HCO absorption lines toward two objects are detected, which almost doubles the number of HCO absorption samples in the Galactic diffuse medium. In addition, high HCO to HCO column density ratios are found, suggesting that the interstellar media (ISM) observed toward the two calibrators are in photodissociation regions, which observationally illustrates the chemistry of diffuse ISM driven by ultraviolet (UV) radiation. These results demonstrate that calibrators in the ALMA Archive are potential sources for the quest for new absorption systems and for detailed investigation of the nature of the ISM.




quasars: absorption lines — ISM: molecules — ISM: abundances — radio lines: ISM

1 Introduction

A molecular absorption system, in which molecular absorption occurs along the line-of-sight toward a radio-loud quasar, is a powerful tool for the investigation of the chemistry and physics of interstellar media (ISM), from those within Galactic diffuse clouds to high-redshift () galaxies. Investigations of the ISM at low excitation states in a distant system indicate higher sensitivity toward absorption than emission ([Wiklind & Combes(1994)]; [Wiklind & Combes(1996)]; [Muller et al.(2011)]), as the absorption line depths are independent of the distance to the system, but dependent on the brightness of the background sources ([Muller et al.(2014)]).


Summary of ALMA archival data in which molecular absorption systems have been found. The objects toward which molecular absorption lines were detected are indicated in bold. Project Observation Band Bandpass Integration Complex gain Integration date calibrator time (s) calibrator time (s) 2011.0.00217.S July 29 - August 1 2012 3 NRAO530 131 J1717337 107 2011.0.00351.S April 7 - July 31 2012 3 J1924292/3C279 421/104 J1717337 333/88 2011.0.00259.S May 8 2012 3 3C279 21 J1625254 55 2011.0.00531.S March 27 - May 4 2012 6 J1924292/3C279 133/132 J1625254 61/61 2011.0.00733.S August 1 2012 3 NRAO530 85 J1604446 69 June 18 - July 4 2012 6 NRAO530 87 J1604446 138 2011.0.00524.S January 12 2012 7 J1427421 103 J1604446 239


List of Galactic molecular absorption systems detected in this work. The objects and detected species indicated in bold are systems and molecules newly detected, respectively. The uncertainty of the absolute flux scales is typically %. Object Galactic coordinates Band Velocity resolution RMS Continuum Detected species in this work name (km s) (mJy) flux (Jy) (Bold: new-detection) c-CH(2–1), HCS(2–1), HCN(1–0), J1717337  352.73 2.39 3 3.4 3 1.4 HCO(1–0), HCO(1–0), HNC(1–0), CH(1–0), HCN(1–0), HCO(1–0), CS(2–1) J1625254 352.14 16.32 3 3.4 7 1.3 c-CH(2–1), CH(1–0), HCN(1–0) 6 1.3 19 0.69 CO(2–1) 3 3.4 6 0.75 CS(2–1) J1604446 335.16 5.76 6 1.3 5 0.39 CO(2–1) 7 0.86 17 0.60 CO(3–2) 3 3.4 1 0.94 HCO(1–0), HCO(1–0), SiO(2–1), NRAO530 12.03 10.81 CH(1–0), HCN(1–0), HCO(1–0) 6 1.3 5 0.77 CO(2–1)

Molecular absorption line systems at high- play an important role in the detection of molecules at high- with high sensitivity, and in investigation of their chemical evolution ([Combes(2008)] (a review); [Wiklind & Combes(1996)]; [Muller et al.(2014)]). In addition, observations of such distant systems can contribute to fundamental physics knowledge by allowing the cosmological variation of fundamental constants or the cosmic microwave background (CMB) temperature as a function of to be probed ([Combes(2008)]; [Henkel et al.(2009)]; [Muller et al.(2011)]). However, note that only four objects are known to have high- molecular absorption at millimeter wavelength ([Combes(2008)]; [Curran et al.(2011)]). Observation of molecular absorption lines in quasar host galaxies also facilitates investigation of gas structures around the active galactic nuclei (AGNs) of edge-on host galaxies ([Roberts(1970)]; [Israel et al.(1991)]; [Espada et al.(2010)]). Furthermore, absorption studies of such host galaxies may be useful in facilitating the direct observation of the putative molecular tori in AGNs, although no detection of this nature has been successfully performed to date ([Okuda et al.(2013)] and references therein).

Even the molecular absorption inside our Galaxy is of considerable interest. Observations of molecular absorption lines in diffuse ISM can improve our understanding of its chemistry. For example, such observations can allow determination of the isotope ratios of fundamental elements based on isotopologue column density ratios ([Lucas & Liszt(1998)]), and may reveal the chemical richness of diffuse ISM by extending the molecular inventory (e.g., [Liszt et al.(2014)]). It is important to investigate the physical and chemical states of diffuse ISM, because such extended diffuse media are thought to be dominant in the interarm regions of our Galaxy ([Sawada et al.(2012)]), and even account for a certain proportion of the total gas in our Galaxy ([Pineda et al.(2013)]). High spatial-resolution observation of the nearby spiral galaxy, M51, also suggests that a diffuse thick disk of molecular gas extends broadly over that galaxy ([Pety et al.(2013)]). Therefore, investigation of the properties of diffuse ISM may even facilitate further comprehension of galactic evolution. However, the detailed nature of diffuse molecular gas is poorly understood, primarily because emission studies experience critical difficulties in detecting such diffuse gases because of their low densities and low excitation temperatures ([Lequeux et al.(1993)]). Several diffuse ISM heating mechanisms have been advocated in previous studies, for example, those based on turbulence ([Godard et al.(2010)]) and UV radiation from OB-stars ([Hollenbach & Tielens(1999)]); however, there exist a limited number of studies observationally supporting such mechanisms from the point of view of the chemical states of diffuse molecular gases. Meanwhile, absorption observations can potentially be used to examine the properties of diffuse ISM.


Absorption line decomposition products of newly detected species. Object Species Frequency LSR velocity Peak optical depth footnotemark: FWHM Column density footnotemark: name (GHz) (km s) (km s) (cm) c-CH(2–1) 85.3389 HCS(2–1) 85.3479 HCN(1–0) footnotemark: 86.3402 HCO(1-0) footnotemark: 86.6708 HCO(1–0) 86.7543 HNC(1–0) 87.0909 J1717337 CH(1–0) footnotemark: 87.3169 HCN(1–0) footnotemark: 88.6318 HCO(1–0) 89.1885 CS(2–1) 97.9810 J1625254 c-CH(2–1) 85.3389 CH(1–0) footnotemark: 87.3169 HCN(1–0) footnotemark: 88.6318 CO(2–1) 230.5380 J1604446 CS(2–1) 97.9810 CO(2–1) 230.5380     footnotemark:     footnotemark: CO(3–2) 345.7960     footnotemark: NRAO530 HCO(1–0) footnotemark: 86.6708 {tabnote} footnotemark: The errors of the peak optical depths and column densities stem from the uncertainty involved in the flux calibration, RMS noise calculation, and line fits.
footnotemark: The data for the molecular lines with hyperfine structure components consist of the strongest values.
footnotemark: Using a rotation diagram with two transition lines, the total column density and of the main CO component are determined to be cm and 6.2 K, respectively, and the of the weaker CO velocity component is also assumed to be 6.2 K, although these results should be treated carefully (see section 3).


Upper limits on peak optical depths and column densities of undetected species. The of all the molecules below are assumed to be 2.73 K. Object Species Frequency Peak optical depth Assumed FWHM Column density ( upper limit) name (GHz) ( upper limit) (km s) (cm) J1717337 HCO(1–0) 85.1622 0.006 5.62 footnotemark: HCN(1–0) 86.0550 0.006 5.62 footnotemark: SiO(2–1) 86.8470 0.005 5.62 footnotemark: HCO(1–0) 87.0575 0.005 5.62 footnotemark: HOC(1–0) 89.4874 0.007 5.62 footnotemark: J1625254 HCS(2–1) 85.3479 0.015 5.78 footnotemark: HCN(1–0) footnotemark: 86.3402 0.015 5.78 footnotemark: HCO(1-0) footnotemark: 86.6708 0.015 5.78 footnotemark: HCO(1–0) 86.7543 0.015 5.78 footnotemark: SiO(2–1) 86.8470 0.015 5.78 footnotemark: CS(2–1) 97.9810 0.017 5.78 footnotemark: CO(2–1) 219.5604 0.163 2.98 footnotemark: CO(2–1) 220.3987 0.196 2.98 footnotemark: J1604446 CS(2–1) 96.4130 0.025 4.32 footnotemark: {tabnote} footnotemark: The data for the molecular lines with hyperfine structure components consist of the strongest values.
footnotemark: The average of FWHM value of all the detected molecular lines toward J1717337.
footnotemark: The average of FWHM value of all the detected molecular lines toward J1625254 in Band 3.
footnotemark: Assuming the same FWHM as the CO(2–1) line toward J1625254.
footnotemark: Assuming the same FWHM as the CS(2–1) line toward J1604446.

However, the number of known molecular absorption systems is rather limited. In regards to Galactic molecular absorption at millimeter wavelength, systems have been noted ([Lucas & Liszt(1996)]; [Lucas & Liszt(2000)]), whereas the lines-of-sight toward a small number of bright sources, such as 3C111, BL Lac, and NRAO530, have been studied extensively (e.g., [Lucas & Liszt(1998)]; [Liszt et al.(2014)]). In addition, previous searches for molecular absorption systems have been limited in terms of sensitivity and velocity resolution. Some of these investigations have reported non-detection (e.g. [Curran et al.(2011)]), even though such studies have been useful in detecting rare molecular species ([Friedel et al.(2011)]).

The advent of the Atacama Large Millimeter/submillimeter Array (ALMA) offers high sensitivity and velocity resolution, allowing researchers to obtain high-quality spectra even within short exposure times. The ALMA archival data offer a vast number of sensitive quasar spectra that have been primarily obtained for bandpass and complex gain calibration. Thus, it is possible that ALMA has detected molecular absorption lines within the spectra of its calibrator sources, and such cases would equate to discoveries of new systems without any additional observation.

In this paper, we present the first results of detections of molecular absorption systems using ALMA calibrator sources. In section 2, we show the data analysis method and, in section 3, we report on the detection of four molecular absorption systems within the Galaxy. In section 4, we discuss the HCO absorption lines, as HCO is the most noteworthy molecule detected in this study.

2 Data Analysis

We select 36 calibrator sources from the whole sky, which fulfill the following criteria: (a) The data are available in the ALMA archive from prior to late 2014, i.e., Cycle 0 data; (b) The continuum flux is detected at Jy, so a high signal-to-noise ratio (S/N) can be expected in Bands 3, 6, or 7; and (c) The data are taken at a frequency resolution of MHz in frequency division mode (FDM). Information on all the sources analyzed in the study is given in Appendix 1. We create three-dimensional (3D) cubes from the calibrated visibilities of the bandpass and complex gain calibrators using the Common Astronomy Software Applications (CASA) package CLEAN task, with Briggs weighting (with a robust parameter of 0.5). Although the spectra of the majority of the calibrators exhibit featureless continua, significant absorption lines () are detected in four objects observed in the six projects listed in table 1. Detailed information on these objects is given in table 1.

When a bandpass calibrator also exhibits absorption lines, the calibration process is performed once more. The bandpass-calibrator frequency channels showing absorption lines (typical widths of km s or MHz) are flagged and linearly interpolated using nearby channels, as interpolation of this nature with a width of MHz does not seriously affect the calibration processes. Then, the revised bandpass calibration is applied so as to yield the final spectrum of the complex gain calibrator. The spectrum of the flux calibrator (the Neptune in this case) to which the interpolated bandpass calibration is applied does not exhibit any artificial features at the frequencies where the lines are found, suggesting that our bandpass interpolation is valid.

The continuum spectrum is subtracted from that of the detected absorption lines using the IMCONTSUB task, and the line spectrum is then divided by the continuum spectrum using the IMMATH task (we have confirmed that the same continuum subtraction is conducted in both the image and planes). Therefore, the line/continuum flux density ratio values are in the - 0 range. The normalized line spectrum is then Gaussian fitted to allow measurement of the central velocity, full width at half maximum (FWHM), and the absorption line depth, which are listed in table 1. The velocity components are identified by comparing the profiles of the hyperfine structure lines and/or the multi-transition lines.

Figure 1: J1717337 and NRAO530 spectra, shown in the top and bottom rows, respectively. The noise level is indicated in a red bar at the top-right of each box (this approach is used hereinafter). The line rest frequencies and intrinsic strength ratios of the hyperfine components of HCO(1–0) and CH(1–0) are shown in the bottom row, from left to right. In the bottom-left box, the line rest frequencies of HCO(1–0) (86.7543 GHz) and SiO(2–1) (86.8470 GHz) are also indicated in bars. Although the lines in the NRAO530 spectra seem to have weak emissions, no sign of emission is confirmed around the source in its 3D data cubes.
Figure 2: Spectra of all molecules detected toward J1717337. The red dotted lines superimposed on the blue solid spectra of HCN(1–0) and HCO(1–0) are the HCN(1–0) and HCO(1–0) spectra, respectively, both of which are multiplied by a factor of 30 (the noise levels indicated by the red dotted bars are those of the C isotopologues, which are also multiplied by 30; those of the C isotopologues are too small to be shown). The intrinsic line strength ratios of the HCN(1–0) hyperfine components are also shown beside the former. An example of a Gaussian fit result, for the HCO(1–0) () absorption line, is shown in an orange dotted line superimposed on the blue solid spectrum. The CH(1–0) ( 3/2–1/2, 2–1) spectrum is represented by the red dotted line, superimposed on the c-CH(2–1) blue solid spectrum. The black bar on the left side indicates the HCS(2–1) line frequency, although the HCS(2–1) detection is marginal and should be treated with some caution.
Figure 3: Spectra of all molecules detected toward J1625254: c-CH(2–1), CH(1–0), HCN(1–0), and CO(2–1), from left to right.

The optical depth and column density of each molecule shown in table 1 are calculated using equations (1) and (2) of Greaves and Nyman (\yearciteGN96) (see Appendix 2 for details), assuming that the excitation temperatures () of the detected molecules are 2.73 K. This means that these molecules are taken to be in equilibrium with the CMB, as has been widely assumed in the previous studies on Galactic molecular absorption systems (e.g., [Greaves & Nyman(1996)]; [Lucas & Liszt(1998)]; [Liszt et al.(2014)]). Further, this has been confirmed for some diffuse media observed toward Galactic star-forming regions ([Godard et al.(2010)]). With this assumption, we can derive optical depths from the line/continuum flux density ratios, which are free from flux calibration uncertainty (%). However, this assumption should be treated with caution if the ISM in question is located in a photodissociation region (PDR, see section 4). Even if is higher than 2.73 K, the measured column density ratios, such as those of (HCO)/(HCO) discussed in section 4, do not change dramatically for molecules with similar . For example, if K, the inferred column densities of all species increase by almost the same factor () for transition from the ground states; this does not change the abundance ratios no more than 10%. Such a discrepancy is negligible compared with the errors associated with the flux calibration, root-mean-square (RMS) noise, and line fits. Further analysis of the impact of and the uncertainty regarding column densities and their ratios will be conducted in a forthcoming paper (Ando et al., in preparation). In addition, the frequency ranges we analyze include the line frequencies of various well-known molecules that are not detected in this work. Table 1 summarizes the upper limits of the peak optical depths and column densities of relatively major undetected species.

3 Results

Of the 36 calibrators analyzed in this work, molecular absorption lines are detected toward the four objects listed in table 1. All of these are found to be Galactic in origin, based on consideration of the line velocities. While the absorption line system found toward NRAO530 has been identified in previous studies (e.g., [Lucas & Liszt(1996)], [Lucas & Liszt(1998)]), the other three systems, toward J1717337, J1625254, and J1604446 are newly detected in this work. The spectra of the four sources are shown in figures 1-4, and each object is described in detail below.

J1717337 is known to exhibit Galactic HI absorption ([Dickey et al.(1983)]), although molecular absorption has never been reported. We detect the ten species shown in table 1, including relatively rare species such as HNC and HCS, all of which are new detections in this system. In addition, four HCO(1–1) and six CH(1–0) hyperfine structure lines are clearly detected. Four velocity components are identified distinctly, as shown in figures 1 and 2. Further discussions of the nature of each molecule detected toward J1717337 and of the C/C isotope ratio will be presented in a forthcoming paper (Ando et al., in preparation).

J1625254 has not been investigated in terms of Galactic absorption, except for a previous search for high- molecular absorption ([Wiklind & Combes(1996)]), with non-detection being reported in terms of this line-of-sight. Hence, all four species reported in this work are new detections. Further, HCO and HCO are not detected, which is significantly different to the profile of J1717337. Only one velocity component is identified, as shown in figure 3.

J1604446 has never been referred to in previous studies. Thus, this is a new Galactic molecular absorption system. As shown in figure 4, absorption lines indicating two CO transitions are detected, with the weaker line corresponding to CS(2–1). Two velocity components are identified in the CO(2–1) spectrum, while only the km/s component is confirmed in that of CO(3–2). Using a rotation diagram with the two transition lines, the of the main CO component is calculated to be 6.2 K. However, this analysis assumes local thermodynamic equilibrium (LTE) and an optically-thin limit, which should be treated carefully in the case of CO lines with moderate optical depths.

NRAO 530 is an extensively-studied Galactic molecular absorption system (e.g., [Lucas & Liszt(1996)]; [Lucas & Liszt(1998)]), but its HCO absorption lines are newly detected (see section 4). A single velocity component is identified, the velocity of which ( km/s) is consistent with the values reported in previous studies ([Lucas & Liszt(1996)]; [Lucas & Liszt(2000)]).

Figure 4: J1604446 spectra. The blue solid and red dotted lines represent the CO(2–1) and CO(3–2) spectra, respectively.

4 Discussion

Figure 5: Column densities of HCO vs. HCO. The column densities measured toward J1717-337 and NRAO530 in this work are plotted in red and orange circles, respectively, with error bars. The data toward 3C111, BL Lac, and W49 (40 km s feature) are from \citetLiszt+14, and are plotted using green symbols. The data for four well-known PDRs (Orion Bar, S140, NGC7023 and NGC2023), which are represented by blue symbols, are from \citetSchilke+01, although (HCO) are derived from (HCO), assuming (HCO)/(HCO) ([Schilke et al.(2001)]). The data for the Horsehead PDR (blue) and Horsehead Cold Core (purple) correspond to the data for the HCO and DCO peaks of the Horsehead Nebula, respectively, which were obtained by \citetGerin+09. As a whole, the filled symbols represent absorption observation results, while open symbols are emission studies data. The red dotted and cyan solid lines correspond to the values of HCO to HCO column density ratios of 19.3 (the average of the ratios measured in diffuse ISM toward the five continuum sources where HCO is detected) and 1 (the threshold of the PDR-like environment in the ISM, [Gerin et al.(2009)]), respectively.

Among the various species detected in this study, HCO is the most noteworthy. Although its emission has been investigated in HII region interfaces ([Schenewerk et al.(1988)]) and in the nearby starburst galaxies, M82 ([García-Burillo et al.(2002)]) and NGC253 ([Martín et al.(2009)]), HCO absorption in diffuse media has only been reported along the lines-of-sight toward two bright quasars (BL Lac and 3C111) and toward the W49 Galactic HII region ([Liszt et al.(2014)]). Therefore, the HCO absorptions toward J1717337 and NRAO530 are the fourth and fifth detections, and this work almost doubles the number of HCO absorption samples in diffuse media.

The detection of HCO absorption itself is quite rare, but it has certain implications. The HCO in diffuse ISM can be used as a PDR tracer ([Schenewerk et al.(1988)]; [Gerin et al.(2009)]; [Martín et al.(2009)]), because of the diffuse media environment. Although there is a moderate density ( cm) of molecular hydrogen (H) gas in a diffuse medium ([Draine(2011)]), such a medium is expected to be illuminated by far-UV (FUV) radiation from distant OB stars ([Hollenbach & Tielens(1999)]). In such conditions, carbon ionized by FUV radiation should be present, as it has been suggested that ionized carbon (C) is the main carbon reservoir in neutral diffuse ISM ([Gerin et al.(2015)]). In a diffuse medium, therefore, it is probable that HCO is formed in the gas phase, through the reaction


([Gerin et al.(2009)]). CH is formed from C and H through several reactions ([Schenewerk et al.(1988)]), and such chemistry is realized in the environment where C and H coexist. Such an environment is comparable to that of classical PDRs, i.e., interface regions between HII regions and molecular clouds ([Hollenbach & Tielens(1999)]). HII regions are directly illuminated by UV radiation, and molecular clouds are dense neutral regions shielded from such radiation.

Furthermore, the (HCO)/(HCO) column density ratio can be used as a diagnostic of the presence of an FUV radiation field, and its high ratio () suggests the presence of ongoing FUV photochemistry ([Gerin et al.(2009)]). Although HCO is known to be sensitive to high-density gas ( cm; [Onishi et al.(2002)]; [Gerin et al.(2009)]), taking the HCO to HCO column density ratio is rather useful in accurately estimating the relative abundance of HCO, because their close proximity in frequency (HCO and HCO at 86.671 and 86.754 GHz) allows us to observe them simultaneously (e.g., [García-Burillo et al.(2002)]; [Liszt et al.(2014)]). Figure 5 shows the HCO and HCO column densities toward the two calibrators, compared with the values measured on the lines-of-sight of the sources toward which HCO absorption was previously detected ([Liszt et al.(2014)]), along with the values in several PDRs ([Schilke et al.(2001)]; [Gerin et al.(2009)]). The (HCO)/(HCO) ratios recorded toward J1717337 and NRAO530 are and , respectively, which are comparable to the values for well-known PDRs ([Schilke et al.(2001)]); this suggests that the media observed toward these sources are in PDR-like environments.

In terms of the heating mechanisms of diffuse ISM, a molecular absorption study has suggested that the gas-phase chemistry of some diffuse media is driven by turbulent dissipation ([Godard et al.(2010)]). Meanwhile, observations of the [CII] fine structure line ([Ingalls et al.(2002)]) and pure-rotational transitions of molecular hydrogen ([Ingalls et al.(2011)]) have demonstrated the role of FUV photons in diffuse media, as it is expected that UV radiation from distant OB stars can penetrate and illuminate diffuse ISM ([Hollenbach & Tielens(1999)]). However, there are a limited number of studies that constitutes observational evidences that FUV photons drive PDR-like chemistry in diffuse molecular gas. This is primarily because, in diffuse ISM, minor molecular species including PDR-tracers cause only minimal emission as a result of their low densities and low excitation states. Therefore, it is remarkable that HCO enhancement comparable to that of PDRs, which suggests a PDR-like environment, is found in diffuse ISM. Importantly, this result observationally illustrates the role of FUV photons in triggering the PDR-like chemistry, and is expected to help us to further understand the heating mechanisms of such media. More detailed investigation into the chemistry and physics of PDR-like diffuse ISM will be presented in a forthcoming paper (Ando et al., in preparation), along with the data on the molecular absorption of higher transition lines, the observation of which is planned in ALMA Cycle 3.

As three Galactic molecular absorption systems are newly detected in this study, the use of ALMA calibrators as potential sources in the quest for molecular absorption systems is proposed. Moreover, the detection of HCO absorption also proves the power of ALMA: just a few minutes’ integration with ALMA almost doubles the number of HCO absorption samples in diffuse media, and provides observational support for the PDR-like chemistry of diffuse ISM processed by FUV radiation. ALMA follow-up observations of the molecular absorption systems that are likely to be discovered through ALMA-calibrator-based searches will constitute not only an efficient manner of investigating the chemical state of Galactic diffuse ISM, but also the best shortcut to extensive comprehension of the detailed nature of ISM as a whole, from our Galaxy to the high- universe.


We thank the anonymous referee for insightful comments, which helped us to improve the paper. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00217.S., 2011.0.00259.S., 2011.0.00351.S., 2011.0.00524.S., 2011.0.00531.S., and 2011.0.00733.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC, ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, NAOJ and NRAO.

Appendix A List of targets analyzed in this work

Table B lists the 36 calibrator sources analyzed in this work, and shows the observation projects that contain these sources and the bands and frequency ranges analyzed in this study, and indicates whether or not absorption lines are detected.

Appendix B Derivation of molecule optical depths and column densities

The peak optical depth of each molecule shown in table 1 is derived from


where is the main beam brightness temperature of the line, is the CMB temperature (2.73 K), is the excitation temperature of the line, is the continuum antenna temperature, and


Equation (A1) is derived from equation (1) of Greaves and Nyman (\yearciteGN96). Note that is negative for an absorption line, as it is defined as the main beam brightness temperature of the line measured in the continuum-subtracted spectrum. As was commonly assumed in the previous studies on Galactic molecular absorption systems (e.g., [Greaves & Nyman(1996)]; [Lucas & Liszt(1996)]; [Liszt et al.(2014)]), we assume that the of the detected molecules is 2.73 K, which has the advantage that can be calculated from the line/continuum flux density ratio in a straightforward manner, because in equation (A1) is offset by .

The total column density of each molecule is calculated from


where is the intrinsic line strength, is the permanent electric dipole moment of the molecule, is the partition function of temperature , and is the lower energy level of the transition ([Greaves & Nyman(1996)]). For each molecule, , which is the conversion factor used to derive the column densities from the integrated optical depths, is shown in table B, assuming a of 2.73 K. As the profile of each line is assumed to be a Gaussian of peak optical depth and FWHM , the integrated optical depths are calculated as


([Godard et al.(2010)]). Therefore the column density of a certain molecule can be derived from the measured and of its absorption line, if is assumed.


List of all targets analyzed in this work.       Object name Project Band                       Frequency range (GHz) Detection J0116-116 2011.0.00099.S 3 112.58-114.46 N J0132-169 2011.0.00061.S 3 96.38-100.25, 108.42-111.29 N J0137-245 2011.0.00172.S 3 85.70-87.57, 87.63-89.40, 97.58-101.32 N J0217+017 2011.0.00083.S 6 341.01-344.70, 352.89-356.64 N 2011.0.00243.S 7 240.25-241.95, 242.61-244.20, 254.65-256.31, 257.09-258.73 N J0334-401 2011.0.00108.S 3 85.40-89.10, 97.27-100.92 N J0339-017 2011.0.00061.S 3 96.07-97.94, 98.07-99.94, 108.11-110.94 N J0403-3605 2011.0.00099.S 3 110.36-112.24 N J0423-013 2011.0.00061.S 3 96.07-97.94, 98.07-99.94, 108.11-110.94 N J0455-462 2011.0.00208.S 7 352.51-354.38, 354.47-356.34, 340.51-342.38, 342.47-344.34 N J0522-364 2011.0.00108.S 3 85.40-89.10, 97.27-100.92 N 2011.0.00099.S 3 108.66-110.53 N 2011.0.00099.S 3 110.83-112.71 N 2011.0.00108.S 7 340.98-344.44, 352.60-356.19 N J0538-4405 2011.0.00170.S 6 233.63-235.51 N J0607-085 2011.0.00170.S 6 216.25-218.84, 233.63-236.02 N 2011.0.00170.S 6 245.32-247.20 N J0637-752 2011.0.00273.S 3 100.09-101.96, 102.05-103.92, 112.21-115.92 N 2011.0.00471.S 3 85.94-86.88, 88.36-89.29, 97.43-98.36, 98.47-99.40 N J0854+201 2011.0.00307.S 7 352.04-353.92 N J0909+013 2011.0.00307.S 7 352.04-353.92 N J1038-5311 2011.0.00497.S 3 84.77-88.34 N J1107-448 2011.0.00497.S 3 84.77-88.34 N J1130-148 2011.0.00497.S 3 86.47-88.34 N 2011.0.00020.S 7 300.01-303.65, 311.94-315.77 N 2011.0.00525.S 7 353.79-355.66 N J1256-057 (3C279) 2011.0.00351.S 3 84.42-88.06, 96.68-100.26 N 2011.0.00121.S 7 319.69-321.56 N J1325-430 2011.0.00121.S 7 319.69-321.56 N J1329-5608 2011.0.00121.S 7 319.84-321.71 N J142739-330612 2011.0.00099.S 3 109.68-111.55 N J1427-421 2011.0.00524.S 3 345.60-346.10 N J1517-243 2011.0.00121.S 7 316.59-318.47, 320.48-322.35 N J1540+147 2011.0.00175.S 7 334.09-335.81, 335.97-337.69, 346.09-349.52 N J1604-446 2011.0.00733.S 3 95.06-98.83, 107.06-108.94, 109.06-110.94 Y 2011.0.00733.S 6 229.61-231.48, 231.60-233.48 Y 2011.0.00524.S 7 344.94-348.23, 356.41-359.62 Y J1625-254 2011.0.00259.S 3 85.16-87.03, 87.05-88.93, 97.16-99.03, 99.05-100.93 Y 2011.0.00531.S 6 219.48-219.61, 220.34-220.44, 230.46-230.56, 232.35-232.48 Y 2011.0.00259.S 7 330.17-332.04, 332.07-333.94, 342.17-344.04, 344.07-345.94 N J1700-261 2011.0.00017.S 3 85.90-87.77 N J1717-337 2011.0.00217.S 3 86.26-88.14, 88.15-90.03, 98.19-100.07, 100.15-102.03 Y 2011.0.00351.S 3 84.42-88.06, 96.68-100.26 Y J1733-130 (NRAO530) 2011.0.00217.S 3 86.26-88.14, 88.15-90.03, 98.19-100.07, 100.15-102.03 Y 2011.0.00733.S 3 95.06-96.94, 96.95-98.83, 107.06-108.94, 109.06-110.94 Y 2011.0.00733.S 6 229.61-231.48, 231.60-233.48 Y J1751+096 2011.0.00526.S 7 334.71-336.59 N J1924-292 2011.0.00108.S 3 85.40-89.10, 97.27-100.92 N 2011.0.00351.S 3 84.42-88.06, 96.68-100.26 N 2011.0.00208.S 7 340.51-342.38 N 2011.0.00526.S 7 334.76-336.63 N J1945-552 2011.0.00046.S 3 99.64-103.35, 111.52-115.23 N J2253+161 (3C454.3) 2011.0.00083.S 7 341.01-344.70, 352.89-356.64 N J2258-279 2011.0.00061.S 3 96.38-98.25, 98.37-100.25, 108.42-111.29 N J2333-237 2011.0.00172.S 3 85.70-87.57, 87.63-89.40, 97.58-101.32 N


Conversion factors used to derive column densities from integrated optical depths, assuming that K. The intrinsic line strengths and permanent electric dipole moments of each molecule, which are used to derive the conversion factors, are taken from \citetMuller+11 and \citetMuller+14, with original reference to data from The Cologne Database for Molecular Spectroscopyfootnotemark: (CDMS) and the Jet Propulsion Laboratory Molecular Spectroscopyfootnotemark: (JPL). Species Frequency Intrinsic line strength Electric dipole moment              Notes (GHz) (debye) (cm km s) HCO(1–0) 85.1622 1.00 3.90 For undetected lines c-CH(2–1) 85.3389 4.50 3.43 HCS(2–1) 85.3479 2.00 1.96 HCN(1–0) 86.0550 1.00 2.99 For undetected lines HCN(1–0) 86.3402 1.00 2.99 HCO(1-0) 86.6708 0.42 1.36 HCO(1–0) 86.7543 1.00 3.90 SiO(2–1) 86.8470 2.00 3.10 For undetected lines HCO(1–0) 87.0575 1.00 3.90 For undetected lines HNC(1–0) 87.0909 1.00 3.05 CH(1–0) 87.3169 0.42 0.80 HCN(1–0) 88.6318 1.00 2.99 HCO(1–0) 89.1885 1.00 3.90 HOC(1–0) 89.4874 1.00 2.77 For undetected lines CS(2–1) 96.4130 2.00 1.96 For undetected lines CS(2–1) 97.9810 2.00 1.96 CO(2–1) 219.5604 2.00 0.11 For undetected lines CO(2–1) 220.3987 2.00 0.11 For undetected lines CO(2–1) 230.5380 2.00 0.11 CO(3–2) 345.7960 3.00 0.11 {tabnote} footnotemark:


  • [Combes(2008)] Combes, F.,  2008, \apss, 313, 321
  • [Curran et al.(2011)] Curran, S. J., et al.  2011, \mnras, 416, 2153
  • [Dickey et al.(1983)] Dickey, J. M., Kulkarni, S. R., van Gorkom, J. H., & Heiles, C. E.  1983, \apjs, 53, 591
  • [Draine(2011)] Draine, B. T.,  2011, Physics of the interstellar and intergalactic medium (Princeton University Press), Ch.1
  • [Espada et al.(2010)] Espada, D., et al.  2010, \apj, 720, 666
  • [Friedel et al.(2011)] Friedel, D. N., Kemball, A., & Fields, B. D.  2011, \apj, 738, 37
  • [García-Burillo et al.(2002)] García-Burillo, S., Martín-Pintado, J., Fuente, A., Usero, A., & Neri, R.  2002, \apj, 575, L55
  • [Gerin et al.(2009)] Gerin, M., Goicoechea, J. R., Pety, J., & Hily-Blant, P.  2009, \aap, 494, 977
  • [Gerin et al.(2015)] Gerin, M., et al.  2015, \aap, 573, A30
  • [Greaves & Nyman(1996)] Greaves, J. S., & Nyman, L. Å.  1996, \aap, 305, 950
  • [Godard et al.(2010)] Godard, B., Falgarone, E., Gerin, M., Hily-Blant, P., & De Luca, M.  2009, \aap, 520, A20
  • [Henkel et al.(2009)] Henkel, C., et al.  2009, \aap, 500, 725
  • [Hollenbach & Tielens(1999)] Hollenbach, D. J., & Tielens, A. G. G. M.  1999, Rev. Mod. Phys., 71, 173
  • [Ingalls et al.(2002)] Ingalls, J. G., Reach, W. T., & Bania, T. M.  2002, \apj, 579, 289
  • [Ingalls et al.(2011)] Ingalls, J. G., Bania, T. M., Boulanger, F., Draine, B. T., Falgarone, E., & Hily-Blant, P.  2011, \apj, 743, 174
  • [Israel et al.(1991)] Israel, F. P., van Dishoeck, E. F., Baas, F., de Graauw, T., & Phillps, T. G.  1991, \aap, 245, L13
  • [Lequeux et al.(1993)] Lequeux, J., Allen, R. J., & Guilloteau, S.  1993, \aap, 280, L23
  • [Liszt et al.(2014)] Liszt, H. S., Pety, J., Gerin, M., & Lucas, R.  2014, \aap, 564, A64
  • [Lucas & Liszt(1996)] Lucas, R., & Liszt, H. S.  1996, \aap, 307, 237
  • [Lucas & Liszt(1998)] Lucas, R., & Liszt, H. S.  1998, \aap, 337, 246
  • [Lucas & Liszt(2000)] Lucas, R., & Liszt, H. S.  2000, \aap, 358, 1069
  • [Martín et al.(2009)] Martín, S., Martín-Pintado, J., & Viti, S.  2009, \apj, 706, 1323
  • [Muller et al.(2011)] Muller, S., et al.  2011, \aap, 535, A103
  • [Muller et al.(2014)] Muller, S., et al.  2014, \aap, 566, A112
  • [Onishi et al.(2002)] Onishi, T., Mizuno, A., Kawamura, A., Tachihara, K., & Fukui, Y.  2002, \apj, 575, 950
  • [Okuda et al.(2013)] Okuda, T., Iguchi, S., & Kohno, K.  2013, \apj, 768, 19
  • [Pety et al.(2013)] Pety, J., et al.  2013, \apj, 779, 43
  • [Pineda et al.(2013)] Pineda, J. L., Langer, W. D., Velusamy, T., & Goldsmith, P. F.  2013, \aap, 554, A103
  • [Roberts(1970)] Roberts, M. S.  1970, \apj, 161, L9
  • [Sawada et al.(2012)] Sawada, T., Hasegawa, T., Sugimoto, M., Koda, J., & Handa, T.  2012, \apj, 752, 118
  • [Schenewerk et al.(1988)] Schenewerk, M. S., Snyder, L. E., Hollis, J. M., Jewell, P. R., & Ziurys, L. M.  1988, \apj, 328, 785
  • [Schilke et al.(2001)] Schilke, P., Pineau des Forêts, G., Walmsley, C. M., & Martín-Pintado, J.  2001, \aap, 372, 291
  • [Wiklind & Combes(1994)] Wiklind. T., & Combes, F.  1994, \aap, 286, L9
  • [Wiklind & Combes(1996)] Wiklind. T., & Combes, F.  1996, \aap, 315, 86
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