A survey of IRAS young stellar object candidates. Searching for large-scale Herbig-Haro objects

Jets and outflows are associated with young stellar objects across the stellar mass spectrum, from brown dwarf protostars to massive, Ae/Be stars. Frequently, the jet morphology is spatially discontinuous because of the temporal variability of the ejection from the driving source. Images covering a wide field of view around the jet driving-source are useful to map the large-scale jet emission and to explore the mass ejection history. The aim of this work was to search for large-scale optical Herbig-Haro (HH) objects lying in a wide field around a sample of IRAS sources, candidates to trace young stellar objects. Deep, narrow-band images through the H$\alpha$ and [SII] emission lines, and through an off-line continuum filter, covering a wide ($\sim15'$) field around the IRAS targets were acquired. The images in the three filters were analyzed to identify shock-excited line emission (i.e., HH) in contrast to scattered line emission. New images of a sample of fifteen IRAS sources, obtained in an homogeneous way are presented. HH emission was detected in six fields, and the astrometry of the knot features is given. The nature of the extended emission as scattered emission around nine of the IRAS targets is confirmed. For seven IRAS sources, with unclear optical counterpart, a more plausible counterpart is proposed. A refined value of the source distance is reported for seven targets. An update of the main data available for each of the sampled fields, including images from public data archives, is also presented.


Introduction
Protostellar jets and outflows are found everywhere in star forming regions as fundamental events occurring during the star formation process. They are believed to regulate processes such as the removal of angular momentum excess from the star-disk system, and the dispersion of the parent cloud. They are observed in all evolutionary stages of young stellar objects (YSOs) where accretion is occurring, from Class 0 to Class III, and across the stellar mass spectrum, from brown dwarf protostars (Whelan et al. 2005;Riaz et al. 2017) to massive, high luminosity young stars (Guzmán et al 2012), and are detected over a wide wavelength range through continuum emission and line emission from molecular, neutral and ionized atomic transitions. Herbig-Haro objects (HHs) are the optical manifestation of outflow events. They are small shock-excited nebulae visible in low excitation lines (eg. [O i], Hα, [S ii]) produced by the radiative cooling in post-shock zones. Most HHs appear as a string of knots aligned in a highly collimated jet (HH-jet) ending in a bright bow-shock where the jet rams into the surrounding medium. The spatial scales covered by the HH-jets range Based on observations obtained at the Centro Astronómico Hispano-Alemán de Calar Alto (CAHA), Spain.
Deceased on 2017 September 27 from a few au, in the case of microjets of T Tauri stars (Agra-Amboage et al. 2011) to several parsecs (giant Herbig-Haro jets, Devine et al. 1999;Reipurth et al. 2019). The knots trace internal shocks driven by velocity ejection variability. Frequently the jet morphology shows discontinuities in its spatial distribution, which is usually attributed to the temporal variability of the ejection material from the source (Raga et al. 1990). Because of this, images covering a wide field of view (FOV) around the suspected driving source are essential to explore the mass ejection history. HH-jets interact with the natal molecular cloud as they travel outwards entraining ambient material and giving rise to large-scale molecular outflows (see e.g., reviews from Frank et al. (2014) and Bally (2016) for a more complete picture of protostellar outflow theory and observations).
We carried out a project aimed at obtaining new deep optical, narrow-band ([S ii] and Hα) images of a sample of IRAS sources, candidates to be tracing YSOs. A sample of fifteen targets was selected to be imaged in a homogeneous way, covering a wide field of view (∼ 15 ) around the IRAS counterpart, looking for shocked emission that could be associated with the target. In addition to the narrow-band images, an image through an off-Hα filter was obtained to get the continuum emission, with the aim of distinguishing between reflected and shocked emission in the neighborhood of each of the sources. Because of the Article number, page 1 of 20 arXiv:2103.01656v1 [astro-ph.SR] 2 Mar 2021 A&A proofs: manuscript no. lopez_37752_c properties of the sources selected, we expected to find HH jets with different evolutionary ages and spatial scales. Most of the fields were not previously imaged through narrow-band filters, nor with a several arcmin wide FOV. Such a spatial coverage is useful to explore whether the HH jet shows discontinuities in its spatial emission, indicative of episodic mass ejections. It was expected that the sample likely included TTauri and Herbig Ae/Be stars being still actively accreting matter from circumstellar disks and driving small scale jets, so that a product of the project would be increasing the sample of known low-mass (TTauri) and intermediate-mass (Herbig Ae/Be) sources driving HH jets. In this work, in addition to the characterization of the optical emission associated with the YSOs traced by the IRAS sources, we updated the observational data available from optical and near-IR data archives for the targets observed, and we performed new accurate astrometry of the jet knots and sources mapped in the observed fields.
The work is structured as follow: in §2 we present the criteria followed to select the sample to be observed; in §3 we describe the observations and data reduction; in §4 we present an updated description of the data available and the results obtained for each of the observed fields, and in §5 we summarize the global results derived from our survey.

Sample selection criteria
The sample observed was extracted from the GLMP catalogues (García-Lario 1991;García-Lario et al. 1997) and the optical survey of Suárez et al. (2006) Suárez et al. (2006) confirm the YSO nature of several YSO candidates of the GLMP sample, based on the optical spectrum of their IRAS counterpart, their luminosity class, and their location in a star-forming region. We selected targets from the GLMP catalogues and the Suárez et al. (2006) survey that, in addition, showed optical emission in the DSS plates. As can be seen in Figures 1 and 2, all of the selected targets have infrared (IR) color indices characteristic of YSOs. Some of the targets are likely to be TTauri or Herbig Ae/Be, which would be visible because they had already emerged from their native environment. Thus, they would still be actively accreting matter from circumstellar disks and could be driving small-scale jets (microjets). The resulting sample consists of fifteen targets that were observable from the Calar Alto Observatory (CAHA) in an observing run during the winter period. Table 1 lists the sample of fields mapped.
According to the nature and morphology of the emission detected in this work (see §4), and the data available in the literature, the sample was separated in three groups, which are indicated in Table 1 and used in Figs. 1 and 2. The first group (I) included fields with extended, pure-line emission, suggestive of being produced by shocked (jet) emission. The second group (II) included IRAS targets associated with nebular, reflected emission. Finally the third group (III) included IRAS targets showing a point-like emission and for which no extended emission, shocked or reflected, was detected in the entire field mapped around the IRAS source. Each observed field is identified with the name of the central IRAS source (listed in column 1) on which the images were centered and its catalogue position is given in columns 2-3. The following columns list the most probably optical counterpart assigned to the IRAS source in the available literature. The classification of the counterpart (Class I, TTauri, FU Ori, Herbig Ae/Be), and the membership of a cluster or extended nebular nature of the object is also indicated.
The rest of columns list the HH objects catalogued in the FOV mapped, the star-forming region where the IRAS source is located, when known, and finally, the distance to the source. Some of the distances have been updated in this work from Gaia data (Gaia Collaboration et al. 2018), and from the improved method based on parallaxes of high-mass star-forming regions of Reid et al. (2019) [60]) color-color diagram. The blue lines mark the region of young stellar objects, and the magenta lines that of ultra-compact H ii regions. Circles correspond to the sources driving jets, squares correspond to the sources with extended nebular emission and triangles correspond to the point-like sources (see Table 1).
As already mentioned, the observed targets have IR colors that are characteristic of YSOs. Figure 1 (Palla 1990), and the region delimited by the magenta lines corresponds to the location of ultracompact H ii regions (Wood & Churchwell 1989), probably associated with YSOs too. Figure 2 presents the (J − H, H − K) CC diagram of the assigned near-IR IRAS counterpart, when known. The J, H, K magnitudes are taken from the 2MASS catalogue 2 .
The region of the plane delimited by the blue square corresponds to the location of TTauri stars (Meyer et al. 1997), the purple lines delimits the region of Herbig Ae/Be (Manoj et al. 2006), and the magenta lines delimits the region of the luminous Class I protostars (Lada & Adams 1992).

Observations and Data Reduction
Observations were carried out on November 2016 with the 2.2 m telescope in the Calar Alto Observatory (CAHA) using the Calar Alto Faint Object Spectrograph (CAFOS) in direct imaging mode. The instrument was equipped with a 2048 × 2048 CCD, giving a spatial scale of 0 . 53 pixel −1 and a field of view of 16 . Three narrow-band filters were used: the line filters of Hα (central wavelength λ = 6569 Å, bandpass ∆λ = 50 Å), and [S ii] 1 http://bessel.vlbi-astrometry.org/node/378, Parallax-Based Distance Calculator V2 2 This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation References. (λ = 6744 Å, ∆λ = 97 Å), which included the emission from the [S ii] λ = 6717, 6731 Å lines, and an off-Hα filter (λ = 6607 Å, ∆λ = 43 Å) to look for the continuum emission nearby to the Hα and [S ii] lines. Conditions were not photometric and the seeing values varied from 1 . 5 up to ∼ 3 during the observing run.
Fourteen fields of our survey were mapped homogeneously in three narrow-band filters, the Hα and [S ii] lines and an off-line, nearby continuum filter. One of the targets (IRAS 05302−0535) was only imaged through the [S ii] filter due to problems during the runs. The images include a total of eighteen IRAS sources. Three fields (centered on IRAS 02236+7224, 03220+3035 and 05380−0728) included a second IRAS source.
We obtained images in Hα and [S ii] of 1 hr of total integration time by combining three frames of 1200 s exposure each, and an additional continuum image of 1200 s integration after combining two frames of 600 s exposure.
All the images were processed with the standard tasks of the IRAF 3 reduction package, which included bias subtraction and flatfielding corrections, using sky flats. In order to correct for the misalignment between individual exposures, the frames were recentered using the reference positions of field stars well distributed around the source. Astrometric calibration of the images was performed in order to compare the optical emission with the positions of the objects reported in the field and, in particular, with the nominal position of the IRAS sources. The images were registered using the (α, δ) coordinates from the USNO Catalogue 4 of ten field stars well distributed in the observed field. The rms of the transformation was 0 . 2 in both coordinates.

Results
In the following, we present the study carried out for each field, following the classification of the sample in the three groups listed in Table 1. The structure of each mapped field is as fol-lows. First, we include a summary updating the relevant information reported in the literature. Next, we detail the new results found from our survey: (i) Wide field image in the narrow-band, off-line continuum filter, with the IRAS source and other YSOs potentially related to the source marked. (ii) Close-ups of selected regions obtained from the images acquired through the Hα and [S ii] line filters. The sub-images allowed us to visualize and characterize the structure of the extended emission around the IRAS source. (iii) For some targets we also show close-ups from images retrieved from public data archives, with the aim of comparing the emission in other wavelengths with the emission detected in our observations. (iv) A table with the detailed astrometry of the shocked emission, if detected. (v) In some cases, we propose a new identification of the IRAS counterpart, based on updated catalogue information and in a more accurate astrometry obtained from our images. IRAS 00087+5833 is located in the dark cloud L1265, in Cassiopeia, at a distance of 344 ± 17 pc (Zucker et al. 2020). In the following we present a short description of the field around the source.
Young stellar objects: They are plotted in Fig. 3 Classified as a deeply embedded object, with neither visible, nor IR emission detected. Has counterparts at 1.3 mm (Henning et al. 1998) and 3 mm (Boissier et al. 2011). Proposed counterpart of IRAS: LkHα 198, but it is offset ∼ 20 from the IRAS position, outside the IRAS error ellipse, as are all the other YSOs. Molecular outflows: Several CO outflows, observed with low (Cantó et al. 1984) and high angular resolution (Matthews et al. 2007   This discards that any of these YSOs could be the counterpart of IRAS 00087+5833. Figure 5 shows a close-up of the Hα and  [S ii] images showing the extended emission associated with the YSOs. We detected line emission from the HH knots HH 161A and HH 461. We did not find any evidence of being related to the IRAS source. Regarding HH 461, the emission of the knot is stronger in Hα than in [S ii], which is a characteristic of the emission from bow shocks. This confirms the nature of HH 461 as a bow shock previously proposed by , based only on geometrical arguments.

IRAS 02236+7224
IRAS 02236+7224 is located in the dark cloud L1340, at a distance of 861 ± 22 pc (Gaia Collaboration et al. 2018). In the following we present a short description of the field around source.
Other IRAS sources in the field: IRAS 02238+7222, in the southern part of the field, with colors that do not correspond to a YSO. Does not seem related to the HHs of the field. Young stellar objects: The RNO 7 cluster of YSOs, with several low and intermediate-mass YSOs surrounded by nebular emission. Proposed counterpart of IRAS 02236+7224: A low-mass, Hαemission star (Kun et al. 2016a) Optical outflows/Herbig-Haro objects: Near IRAS 02236+7224: Jet in Hα and [S ii] emerging southwards from IRAS (Nanda . Knots of the jet : HH 671A and B: most probably associated with the cluster, but not clearly related to IRAS. Knot 3: located ∼ 1 southwest of HH 671B, close to a bright Hα emission star. Knot 5: HH 672 in the Reipurth et al. (2000) catalogue, located ∼ 3 southwest of IRAS. HH 488: Chain of emission knots, in the east-west direction, south of IRAS 02238+7222, observed in [S ii].
-Exciting source not established up to now.
-Different nomenclatures of the knots, as reported by Nanda , Magakian et al. (2003), and in the Reipurth et al. (2000) catalogue (see Table  3 for the cross-identifications based on the astrometry of the present work). -IR counterparts of HH 488 and J optical knots and new knots HH 488E to G without optical counterpart from Spitzer images (Kun et al. 2016b). Near-IR counterparts (H 2 2.12 µm line) catalogued by Walawender et al. (2016) as MHO objects (see Table 3).  cluster can be seen at the center of the image, and the location of the two IRAS sources are also marked. Our narrow-band images allowed us to identify the optical knots HH 671A and B, the chain of knots HH 488A to D, the J complex northwest of IRAS 02238+7222, and the HH 672 knot, ∼ 3 southeast of IRAS02236+7224. In addition, we detected a new knot ∼ 20 west of HH 671A, labelled H in our images, which corresponds to the optical counterpart of MHO 2932B.   Regarding the cross-identification of the optical and near-IR knots of HH 488, and the J complex, we show in Fig. 9 the colorcomposed image from the Spitzer archive, where these knots have been marked with the labels listed in the first column of Table 3.
We made accurate astrometry of all the knots detected in our images, necessary to determine the positions of the jet knots and the relationship between the optical and near-IR knot emissions in a consistent way, including the MHOs features reported by Walawender et al. (2016). Table 3 lists the positions for all the HHs knots mentioned here. Since we found discrepancies in the identifications of several knots of the field, the table displays the knots identification of Nanda  and Magakian et al. (2003), and the identification in the Reipurth et al. (2000) catalogue. The table also displays the H 2 MHO counterpart of each knot ).  IRAS 03220+3035 is located in L1448, in the Perseus cloud complex, at a distance of 240 ± 12 pc (Zucker et al. 2020). In the following we present a short description of the field around the source.
Proposed association of IRAS with other objects: RNO 13: Red reflection nebula (Cohen 1980), and A&A proofs: manuscript no. lopez_37752_c  (194,195,196) are identified (top), and the knots listed in Table 4 are labeled, enclosed in boxes (bottom).
-Very embedded, with no optical nor near-IR counterpart. -Classified as a Class 0 protostar, from far-IR and submillimeter data (O'Linger et al. 1999). IRAS 03225+3034 IRS3, associated with YSOs (Anglada et al. 1989), but outside the field mapped. Binarity: L1448 IRS1 is a close (1 . 37) binary system (L band images of Connelley et al. 2008 Figure 10 shows the wide field mapped in the continuum filter. The location of the IRAS sources included in the field are marked. Figure 11 is a close-up of the field mapped through the Hα and [S ii] narrow-band filters. The images show the location of HH 194,HH 195,and HH 196 (Hα image), and the knots identified in our [S ii] image, which have been labeled beginning with A, the knot closest to the proposed driving source.
None of these HH objects is aligned with IRAS 03222+3034 (our target), so there is no clear geometric argument to associate the driving source of any of the HH objects with the IRAS source.
Let us discuss each HH object in more detail. Astrometry of the HHs 194,195 and 196 knots, including the newly identified substructures, is given in Table 4.

IRAS 04073+3800
IRAS 04073+3800 is located in the dark cloud L1473 in the Perseus complex, at a distance of ∼ 350 pc (Cohen et al. 1983). In the following we present a short description of the field around the source.
Proposed association of IRAS with other objects: PP 13, an optical red nebula with a position closely matching that of IRAS (Parsamian & Petrossian 1979 Table 5 are labeled (bottom). The positions of the two red nebulous objects (PP 13N and S) are marked as in Fig. 12.  [S ii] observations of . The astrometry of the knots of the [S ii] image is given in Table 5. As can be seen in Fig. 13, most of the knots are brighter in [S ii] than in Hα. The exceptions are knot A of HH 464, the knot closest to the exciting source, and the line emission features X1/2 and Y, associated with HH 463, which are brighter in Hα than in [S ii]. In the case of HH 463X1/2 and Y, their position far away from the exciting source and their disordered morphology suggest that they may be tracing bow shocks from older mass-ejection episodes.
The field close to IRAS 04073+3800 was imaged by the HST with the WPC2 camera through the F814W filter (PI D. Padgett. Program ID 9160. Cycle 10) and with the NIC2 camera through the filter F110W, F160W and F205W (PI D. Padgett. Program ID 10603. Cycle 14). Figure 14 shows a close-up of the F814W image.
We identified three knotty structures (N1, N2, N3) south of PP 13N at a PA 25 • , and another three knots (S1, S2, S3) south of PP 13S at a PA 35 • . The astrometry of these knots, derived from the HST image, is given in Table 6. The S knots are part of the HH 463 jet. Given their positions, we could identify S1 with HH 463A, while S2 and S3 correspond to HH 463B, resolved in different substructures because of the better resolution of the HST image.
Regarding the N knots, they are well aligned with HH 465A (PA 20 • ), so they could be part of the jet/counterjet system powered by PP 13N. However, they are also aligned with the S knots of the HH 463 jet, which shows a curved morphology at large scales. Thus, they could also trace the counterjet of HH 463, projected onto the PP 13N nebula.

IRAS 04239+2436
IRAS 04239+2436 is located in the B18 cloud of Taurus, at a distance of 129.0 ± 0.8 pc (Galli et al. 2019). In the following we present a short description of the field around the source.
Classification: Low-luminosity Class I protostar, from its near-IR spectrum (Greene & Lada 1996). Binarity: Close binary (separation 0 . 3, 42 au in projection) (Reipurth 2000). Molecular outflows: CO outflow driven by IRAS (Moriarty-Schieven et al. 1992). Optical outflows/Herbig-Haro objects: Giant HH bipolar outflow HH 300 (Reipurth et al. 1997), driven by IRAS. -Jet emission in [Fe ii] collimated and bipolar (Davis et al. 2011), with axis coincident with the optical HH 300A-C knots axis (Reipurth 2000). -Jet emission in H 2 collimated and bipolar (Davis et al. 2011). -Jet emission in Brγ isotropical (Davis et al. 2011). The field of our images centered on IRAS 04239+2436 did not include the bright redshifted HH 300A, B and C knots. Figure 15 shows the field imaged in the continuum filter with the location of the IRAS source. Figure 16 shows a close-up of the field surrounding IRAS 04239+2436 through the Hα and [S ii] line filters. As can be seen in the figure we detected emission in the two lines from two knots of the blueshifted HH 300 jet. In the Hα+[S ii] image of Reipurth et al. (1997), HH 300D shows a conical shape, reminiscent of a bow-shock. Our images revealed that the morphology of knot D changes from Hα to [S ii]. In the Hα line, knot D shows the bow-shock shape reported before, while in the [S ii] line knot D appears split in two (labeled DE and DW in  4.1.6. IRAS 05380−0728 IRAS 05380−0728 is located in the southern region of the L1641 molecular cloud, at a distance of 460 pc (Cohen 1990). In the following we present a short description of the field around the source.
Luminosity: One of the most luminous objects of the cloud. Estimated total luminosity of 250 L (Reipurth & Bally 1986). Association of IRAS with other objects: IRS1, in the western edge of the reflection nebula Re50N, a very red point-like source (Casali 1991).
-Detected in the near-IR (J, H, K, L bands).
-Variability: from 2006 to 2014, Re50N increased its brightness while Re50S faded significantly, probably caused by dusty material orbiting the sources (Chiang et al. 2015). Optical outflows/Herbig-Haro objects: SMZ9-4, 5 and 6: a large-scale strand of knots and filaments in the H 2 line at 2.12 µm (Stanke et al. 2000). Driven by a different source, IRAS 05380-0731. HH 65: faint, single knot in [S ii] (Reipurth & Graham 1988), located at the red lobe of a bipolar CO outflow. It is the optical counterpart of SMZ9-6. HH 1121: a knotty chain north of the Re50S nebulosity (Chiang et al. 2015). HH 1122: two faint knots ∼ 1 southwest of Re50S (Chiang et al. 2015). Fig. 17 displays the field centered on IRAS 05380−0728 imaged trough the continuum filter. Another IRAS source, IRAS 05380-0729, appears also in the image. IRAS 05380−0728 is located at the tip of Re50N. In our image, both Re50N and Re50S appear with a similar brightness. Re50N has an 'S' shape, while Re50S has an arrowhead shape. The same morphology is found in the Hα and [S ii] filter images (Fig. 18).
Regarding the variability of Re50N and Re50S, both nebulosities keep the same shape as observed in the [S ii] image of 2014 (Chiang et al. 2015). However, in our [S ii] image (Fig. 18) Re50N and Re50S have a similar brightness, and Re50S is not dimmer than Re50N as reported in 2014 (Chiang et al. 2015). Concerning the HH objects of the region, we detected HH 65 in the Hα and [S ii] images. We found a slightly different morphology in Hα and [S ii]: the knot is more compact and brighter in [S ii] than in Hα. HH 1121 was only detected in the [S ii] image. In contrast, HH 1122 was detected in both emission lines, being brighter in Hα than in [S ii]. We did not detect any additional emission line features in our deep narrow-band images of this region.

IRAS 00044+6521
IRAS 00044+6521 belongs to the Cepheus IV association, at a distance of 845 ± 110 pc (MacConnell 1968). In the following we present a short description of the source.
Proposed IRAS counterpart: -The optical object appears as a Herbig Ae/Be of the Herbig & Bell (1988) catalogue as HBC 1. -Also known as the emission star MacC H12 (MacConnell 1968), with Hα line emission (Cohen & Kuhi 1976). -Included in the Herbig Ae/Be survey of Thé et al. (1994), and classified with a spectral type around F4 (Hernández et al. 2004). -Broad-band (R, I, J, H, K, L) images (Origlia et al. 1990) show a red stellar component and a nebula, consistent with a TTauri star with an accretion disk and a cold dust envelope. -Its position is offset ∼ 5 from the IRAS position. Figure 19 shows the image of the field around IRAS 00044+6521 through the continuum filter, and Fig. 20 shows close-ups of the Hα and [S ii] lines filter images.
As can be seen in the figures, the target shows a compact emission, inside the position error ellipse of IRAS 00044+6521, plus a cometary tail ∼ 10 long, extending southeastward. The extended emission has the same shape in continuum and line emission, thus confirming that the origin of the emission is most probably scattered light, and not shock excitation from a stellar microjet. We measured an offset of 6 . 5 between the nominal position of the IRAS source and the 2MASS source J00070260+6538381, the 2MASS source coinciding with the photocenter of the compact optical counterpart. Figure 21 shows a close-up of the field around IRAS 00044+6521 from the HST ACS/WFC image through the F814W filter, extracted from the HST Legacy Archive (PI Sahai. Program ID: 10536). The extended emission can be seen in more detail, showing an arc-shaped morphology, with its center toward the IRAS position. The proposed optical/near-IR counterpart of IRAS lies at the northwest tip of the nebulosity.

IRAS 05302−0537
IRAS 05302−0537 is located at the southern part of Orion A, at a distance of 319 ± 17 pc (Gaia Collaboration et al. 2018). In the following we present a short description of the field around the source.
First proposed counterpart of IRAS: Haro 4-145, an Hα emission star (Parsamian & Chavira 1982). Present proposed counterpart of IRAS: K-band reflection nebula: point-like counterpart with a diffuse nebula extending northwards from the near-IR source (Connelley et al. 2007). with IRAS. Source slightly elongated in the northeastsouthwest direction (consistent with its binary nature, see below), surrounded by diffuse, arc-shaped emission extending from northwest to southeast of the compact source. Binarity: Binary system with an angular separation of 0 . 65 (Lband images; Connelley et al. 2008).
Due to weather conditions, only the narrow-band [S ii] image of the IRAS 05302−0537 field was obtained in our CAHA survey (Fig. 22). We barely detected a faint, compact emission coinciding with the IRAS source, but we did not detect any extended emission associated with it. Our image also shows another YSO, Haro 4-145. This object is in a more evolved stage than J05324165-0535461, as indicated by its near-IR colors, and the lower extinction allowing to be detected at optical wavelengths. Haro 4-145 lies ∼ 25 southeast of the IRAS source position, outside the IRAS error ellipse. Thus, it is unlikely to be the optical counterpart of the IRAS source. Instead, J05324165-0535461 is more likely to be the IRAS counterpart. Haro 4-145 is marked with a white "+". The IR source Vision J5324165−0535461 (Meingast et al. 2016) is marked with a red "+", nearly overlapping the black "+" of the IRAS source.

IRAS 05393+2235
IRAS 05393+223 is located at a distance of 1540 ± 106 pc (Gaia Collaboration et al. 2018). In the following we present a short description of the source.
-Associated with extended emission (Cohen 1980) with a cometary-shape morphology (broad-band, R filter image; Goodrich 1987), -FU Ori star, with a spectral type F5 II (Goodrich 1987). -Probable post-FU Ori star (double Li absorption profile; Torres et al. 1995). Figure 23 shows the IRAS 05393+2235 field in the continuum filter and Figure 24 shows close-ups in the Hα and [S ii] line filters. As can be seen in the figures, the extended, arcshaped nebulosity surrounding the compact counterpart of the IRAS source presents the same morphology in the continuum and in the line images, indicating that the extended emission is most probably a reflection nebula. No evidence of shocked gas was found in our narrow-band images.

IRAS 06249−1007
IRAS 06249−1007 is located at a kinematic distance of 0.86 ± 0.07 kpc (see Footnote 1), determined from its radial velocity, V LSR = 12.2 km s −1 (Wilking et al. 1989). In the following we present a short description of the field around the source.

Optical and IR emission:
-IRAS located ∼ 10 from the southwest edge of the loopshaped nebula HHL 43 (Gyulbudaghian 1984). -HHL 43 has the same loop-shaped morphology in broadband optical (I) and near-IR (J, H, K) images (Tapia et al. 1997). -Emission at 100 µm peaking at the nominal position of IRAS (Di Francesco et al. 1998). Young stellar objects: -A cluster of four stars, all inside the IRAS error ellipse, with near-IR colors characteristic of embedded TTauri stars (Tapia et al. 1997).  be seen in the figures, the nebula shows the same morphology in continuum and in the line images, indicating that the origin of the emission is mainly reflection (dust illuminated by the cluster of stars), without signs of shocked emission. In our images, the cluster of YSO including the IRAS counterpart lies outside the nebular emission. We did not detect any optical counterpart of any of the YSO of the cluster. This is consistent with an extinction increasing from north to south along the nebula (Tapia et al. 1997), with the YSO cluster being embedded in extended K-band emission.

IRAS 06562−0337
IRAS 06562−0337 is located at a kinematic distance of 5.65 ± 0.43 kpc (see Footnote 1), determined from its radial velocity, V LSR = 54.0±0.2 km s −1 (Bachiller et al. 1998). In the following we present a short description of the field around the source. -Renamed as Iron-clad Nebula, and classified to be in a transition phase from AGB to PN, based on its high variability and spectrum dominated by allowed and forbidden Fe ii lines (Kerber et al. 1996). Association of IRAS with molecular gas: CO, 13 CO, and CS emission at millimeter and sub-millimeter wavelengths (Bachiller et al. 1998). -Powering source of a molecular outflow traced by the high-velocity CO emission. -Non-evolved object because the CS molecule is destroyed in the proto-PN stage. Association of IRAS with IR emission: K -band image of the field (Alves et al. 1998).
-IRAS is a young, rich stellar cluster embedded in diffuse emission. -The cluster contains ∼ 70 stars within a 30 radius around the bright central object. -The central object is likely a Herbig Be star.
-Spectral variability of the central object attributed to a stellar wind in its extended atmosphere. -The coordinates of the central source in the K -band image are in agreement with the CO emission peak. Figure 27 shows the IRAS 06562−0337 field mapped through a continuum filter, and Fig. 28 shows close-ups of the Hα and [S ii] line filter images, where the stars of the IR cluster have been marked. We did not detect any nebular, shocked emission from jet structures.

IRAS 00422+6131
IRAS 00422+6131 is located at a distance of 2400 +920 −520 pc, derived from its parallax (Gaia Collaboration et al. 2018). In the following we present a short description of the field around the source.

Controversial nature of IRAS:
-The source lies in projection toward the young open cluster NGC 225, although it is not a member of it (Lattanzi et al. 1991). -First identified as a TTauri star on he basis of its IRAS colors .  Figure 29 shows the image of the IRAS 00422+6131 field through a continuum filter. Close-ups of the narrow-band images in the Hα and [S ii] line filters are shown in Fig. 30.
All the images show a similar morphology of the IRAS optical counterpart. We did not detect in our narrow-band line images any shocked emission from jet structures.

IRAS 02181+6817
IRAS 02181+6817 is located at a distance of 664 ± 25 pc (Gaia Collaboration et al. 2018). In the following we present a short description of the source.
Proposed IRAS counterpart: An optical/near-IR bright star.
-Classified as a TTauri star, based on the IRAS colors (García-Lario 1991). -Reported as a non-periodic variable star, CO Cas (Hoffmeister 1936;Samus et al. 2017), with an average V mag = 15.52, and a variation amplitude of 1.15 mag (Kochanek et al. 2017  We found two sources located less than 5 from the IRAS position, inside the IRAS error ellipse. The brighter source is CO Cas, the proposed IRAS counterpart. The other source is located a few arcsec southeast of CO Cas (labeled as 3 in Fig. 32). The source is faint and slightly elongated in the northwest-southeast direction, and could be tracing a micro-jet powered by CO Cas.

IRAS 05426+0903
The optical counterpart of IRAS 05426+0903 is the prototypical, young pre-main sequence star FU Ori. It is located at a distance of 416 ± 9 pc (Gaia Collaboration et al. 2018). In the following we present a short description of the source.
-FU Ori S is an actively accreting young star, withṀ acc (2-3)×10 −8 M yr −1 , and is the more massive component of the binary system (Beck & Aspin 2012). -Continuum emission at 1 mm detected from circumstellar disk (Hales et al. 2015). -High-density tracer HCO + emission-peak close to FU Ori S, indicating that it is embedded in dense molecular gas (Hales et al. 2015).

Circumbinary reflection nebula:
-Detected through near-IR, high-resolution imaging polarimetry (Liu et al. 2016;Takami et al. 2018). -Arc-like morphology, reminiscent of a spiral arm stretching from east to northeast of the FU Ori system. -Morphology probably caused by gravitational instabilities in the accretion disks, in an unstable phase of protoplanetary disk evolution. Figure 33 shows the IRAS 05426+0903 field mapped through a continuum filter. Close-ups of the narrow-band images in the Hα and [S ii] line filters are shown in Fig. 34. All the images show a similar morphology of the IRAS optical counterpart. We did not detect shocked emission from jet structures in our narrow-band line images.

IRAS 06471−0329
IRAS 06471−0329 is located near the CO boundary of G216−2.5, at a distance of 2110 ± 21 pc (Zucker et al. 2020). In the following we present a short description of the source.
First proposed counterpart of IRAS: A red star detected in the I-band (Campbell et al. 1989). Later proposed counterpart of IRAS: One of the two bright stars in the K-band, close to the IRAS position (Lee et al. 1996).
-Very high reddening, with near-IR colors consistent with those of embedded YSOs. -Associated with an IR nebulosity (Ishii et al. 2002).
-Absorption feature at 3.1 µm from H 2 O ice, usually present in high-density interstellar clouds protected from UV radiation, characteristic of embedded objects. Figure 35 shows the image of the IRAS 06471−0329 field through a continuum filter. Close-ups of the narrow-band images in the Hα and [S ii] line filters are shown in Fig. 36. We detected in all the images a weak nebular emission surrounding three point-like sources southwest of the bright star at the center of the field. This weak reflection nebula should correspond to the near-IR emission detected by Lee et al. (1996) and Ishii et al. (2002). In the narrow-band line images (Fig. 36) we show the catalogue positions of the IRAS source (white) and the 2MASSX source J06494021−0332523 (red). As can be seen in Fig. 36, the position of the 2MASSX source coincides with a weak star surrounded by nebular emission. Thus, we concluded that the optical counterpart of IRAS 06471−0329, instead of being the bright star at the center of the field, is most probably the more embedded near-IR source J06494021−0332523.

Conclusions
We obtained narrow-band images covering a wide FOV around a sample of IRAS sources that were proposed to be associated with YSOs, based mainly on their location in CC diagrams. The association of the IRAS source with young stellar objects has been confirmed from the images obtained. Although these fields were observed in the past, our survey provides new data both for the IRAS counterparts themselves and for their environment. In particular: -In this survey, the first-ever images through the narrowband, Hα and [S ii], line filters were obtained for nine IRAS sources (all the targets of groups II and III). The IRAS sources of group II were known to have extended emission. However, previous imaging was only made through broadband filters, which do not allow to distinguish with confidence between reflected and shocked emission. The narrowband images obtained confirm the nature of the extended component of the emission associated with the targets. In IRAS 02181+6817, a point-like target of group III, an elongated emission in the Hα and [S ii] lines was detected, southeast of the source, which could be tracing a micro-jet powered by the source. -New images in the two emission lines, Hα and [S ii], were obtained for three sources of group I (IRAS 03220+3035, 04073+3800, and 04239+2436) These sources were previously mapped only in one of the lines, or through a broadband, red continuum filter. -In six of the mapped fields (group I), extended emission in the Hα and [S ii] lines was detected, with no continuum counterpart, tracing HH jets. In some targets (IRAS 00087+5833, 02236+7224, and 03220+3034), the jet emis- sion was not associated with the IRAS target, but with another YSO in the mapped field. -The astrometric positions of most of the jet knots were not reported in the literature. Astrometry of the jet knots mapped in our images was performed, and is given in the section corresponding to each source. In addition, new substructures were resolved within the knots of the jets of HH 196A and HH 196B, imaged in the field of IRAS 03220+3035, and HH 300, powered by IRAS 04239+2436. Two new knotty emissions, closer to the IRAS source, labeled HH 300D0 and D1, were identified in the images. -For three of the observed fields (IRAS 00087+5833, 02236+7224, and 04073+3800) we were able to identify jet knots in previous optical and near-IR images in public archives (HST, Spitzer). Their positions were compared with our results from the CAHA observations, and near-IR counterparts of some knots were identified. -We confirmed or proposed a different IRAS counterparts for seven targets of the sample (IRAS 00044+6521, 00087+5833, 04073+3800, 05302−0537, 05393+2235, 06249−1007, and 06471−0329). To sustain these associations, the astrometric positions of the YSOs in the neighborhood of the target source were obtained.