Stellar Overdensity in the Local Arm in Gaia DR2

Using the cross-matched data of Gaia DR2 and 2MASS Point Source Catalog, we investigated the surface density distribution of stars aged ~1 Gyr in the thin disk in the range of 90{\deg}<= l<= 270{\deg}. We selected 4,654 stars above the turnoff corresponding to the age ~1 Gyr, that fall within a small box region in the color-magnitude diagram, (J-Ks)0 versus M(Ks), for which the distance and reddening are corrected. The selected sample shows an arm-like overdensity at 90{\deg}<= l<= 190{\deg}.This overdensity is located close to the Local arm traced by high-mass star forming regions (HMSFRs), but its pitch angle is slightly larger than that of the HMSFR-defined arm. Although the significance of the overdensity we report is marginal, its structure poses questions concerning both of the competing scenarios of spiral arms, the density-wave theory and the dynamic spiral arm model. The offset between the arms traced by stars and HMSFRs, i.e., gas, is difficult to be explained by the dynamic arm scenario. On the other hand, the pitch angle of the stellar Local arm, if confirmed, larger than that of the Perseus arm is difficult to be explained with the classical density-wave scenario. The dynamic arm scenario can explain it if the Local arm is in a growing up phase, while the Perseus arm is in a disrupting phase. Our result provides a new and complex picture of the Galactic spiral arms, and encourages further studies.


INTRODUCTION
Revealing the shapes of spiral arms in the Milky Way is a long-standing challenge in Galactic astronomy (e.g. Vallée 2017). First successful identification of spiral arms in the Milky Way has been made by Morgan et al. (1952) from distributions of ionized hydrogen in the so-lar neighborhood. Since then, many studies have reported the characteristics of spiral arms in the Milky Way (e.g., van de Hulst et al. 1954;Oort et al. 1958;Georgelin & Georgelin 1976;Russeil 2003;Paladini et al. 2004;Hou & Han 2014). The well-known spiral arms within a few kiloparsecs of the Sun are the Sagittarius-Carina arm and the Perseus arm. The Sagittarius-Carina arm passes Galactic longitude of l = 0 • inside the solar radius, and the Perseus arm passes l = 180 • outside the solar radius. These features are revealed by a large number of gas and young stellar tracers, such as O and early B stars, giant molecular clouds and H II regions (Bok et al. 1970;Russeil 2003;Hou et al. 2009;Hou & Han 2014;Monguió et al. 2015). The Perseus arm is also associated with the excess of older stars (Churchwell et al. 2009, and references therein). On the other hand, such an excess of old stars has not been found around the Sagittarius arm (Benjamin et al. 2005). These lead to an ongoing debate that the Perseus arm could be one of two major spiral arms in the Milky Way, while the Sagittarius-Carina arm is a minor gaseous spiral arm (Drimmel 2000;Benjamin 2008;Churchwell et al. 2009). Spiral patterns in the Galactic plane are also traced by high-mass star-forming regions (HMSFRs) whose precise parallaxes can be measured using Very Long Baseline Interferometry (VLBI; Reid et al. 2009;Honma et al. 2012;Reid & Honma 2014). More than 100 HMSFRs have been identified at the expected locations of the Sagittarius-Carina and Perseus arms .
There is another closest spiral arm between the Sagittarius-Carina and Perseus arms. This spiral arm is called the "Local arm" and also called the "Orion Arm" (van de Hulst et al. 1954;Georgelin & Georgelin 1976;Xu et al. 2016). The Local arm is identified with the neutral hydrogen gas, H II regions, Cepheids, OB stars and HMSFRs (Walraven et al. 1958;Bok 1959;Becker & Fenkart 1970;Hou & Han 2014;Xu et al. 2016Xu et al. , 2018b. However, the features of the Local arm is not very clear, compared to the Sagittarius-Carina and Perseus arms. The Local arm is often considered to be a branch-like features or a spur which bridges between the Sagittarius-Carina arm and the Perseus arm (Oort & Muller 1952;Morgan et al. 1953;van de Hulst et al. 1954;Kerr 1970;Kerr & Kerr 1970;Russeil 2003;Russeil et al. 2007;Xu et al. 2016Xu et al. , 2018b. This infers that the Local arm is not a major spiral arm, but a secondary minor spiral feature, which is just connected patchy star forming regions only traced by gas and very young stars (Gum 1955;Bok 1959;Bok et al. 1970;Kerr 1970;Georgelin & Georgelin 1976;Hou & Han 2014). However, a large number of HMSFRs are observed in the Local arm, and the overall length (> 5 kpc) identified with HMSFRs is substantial, which led to a recent debate that the Local arm may be a major spiral arm (Xu et al. 2013(Xu et al. , 2016. If the Local arm is a major spiral arm, we should be able to identify the stellar overdensity of the Local arm, which has not been observed, despite its being the closest spiral arm. The European Space Agency's Gaia mission (Gaia Collaboration et al. 2016) has made their second data release (Gaia DR2;Gaia Collaboration et al. 2018). Gaia DR2 provides the position, parallax and proper motions for ∼ 1.3 × 10 9 stars in the Milky Way (Lindegren et al. 2018), and radial velocity for about 7 million stars (Soubiran et al. 2018) measured with Radial Velocity Spectrograph (RVS; Cropper et al. 2018). The precise measurement of the parallax for the bright stars around the Local arm in Gaia DR2 enables us to study the stellar distribution for a selected population of stars. In this paper, to answer the question if or not there is a stellar arm associated with the Local arm, we map the stellar density of a specific population of stars with about 1 Gyr of age at 90 < l < 270 • . The 1 Gyr population is chosen, because they are significantly older than the previously known Local arm tracers and they are bright and more uniquely located in the Hertzsprung−Russell (HR) diagram. Cross-matched sample of Gaia DR2 stars with the Two Micron All Sky Survey Point Source Catalog (2MASS PSC; Skrutskie et al. 2006) are used to identify the population. We also evaluated the completeness of our selected sample against the 2MASS PSC, and confirmed that our sample has reasonable completeness within the distance of 0.2 and 1.3 kpc.
If the stellar arm is identified, the positional offset between the gas and stellar arms, it would be interesting to consider the origin of the spiral arm (Dobbs & Pringle 2010;Baba et al. 2015;Egusa et al. 2017). Recently, the origin of the spiral arms is hotly debated. There are two major competing scenarios for isolated spiral galaxies (see a review by Dobbs & Baba 2014). One of them is a classical density-wave scenario, where the spiral arms are considered to be long-lived and rigidly rotating density wave features (Lin & Shu 1964, 1966Bertin & Lin 1996). The other one is a transient dynamic spiral arm scenario, which is commonly seen in N -body simulations of disk galaxies. In this scenario, the spiral arm is short-lived, transient and recurrent (Sellwood & Carlberg 1984;Fujii et al. 2011;D'Onghia et al. 2013), and the arm is co-rotating and winding with the stars at every radius (Wada et al. 2011;Grand et al. 2012a;Baba et al. 2013). This is also the case for barred spiral galaxy simulations (Baba et al. 2009;Grand et al. 2012b;Baba 2015). In the density-wave scenario, the stellar arm is expected to have different degrees of offset from the gas arm at different radius (e.g . Fujimoto 1968;Roberts 1969;Gittins & Clarke 2004), and hence the gas and spiral arms have different pitch angles (e.g. Pour-Imani et al. 2016). On the other hand, the dynamic spiral arm scenario predicts no systematic offset of the gas and stellar arms, because they are co-rotating with each other (Grand et al. 2012a;Kawata et al. 2014;Baba et al. 2015).
This paper investigates the stellar overdensity in the Local arm and the offset of the stellar arm from the gas arm identified with the HMSFRs. Section 2 describes our selection of the 1 Gyr age stellar population and discusses the distance range where the selected population shows reasonable completeness. Section 3 shows our results. Summary and discussion are provided in Section 4.

DATA
The data used in this paper are described in this section. We first explain how we selected our sample of stars to analyze the surface stellar density map around the Local arm in Section 2.1. Then, in Section 2.2 we describe the maser sources associated with HMSFRs, which are used to define the location of the Local arm for the star forming regions, i.e. gas. We assumed the solar radius of R 0 = 8.34 kpc ) in this paper.

Stellar Data
In this paper we focus on the stellar population with the age of around 1 Gyr, and measure the surface density map to test if there is any stellar overdensity in the Local arm. Although the age of 1 Gyr is a relatively young age, they are older than the populations which are used to identify the Local arm in the past, and we consider that it is old enough to represent the stellar mass distribution of the Galactic thin disk stars. Also, the relatively young stellar population was chosen, because the color and magnitude ranges of their turn-off stars are more isolated in the HR diagram. In this paper, we focus on the region of the Galactic longitude between l = 90 • and l = 270 • , because the dust extinction is less severe and a clear excess of the HMSFRs is observed and identified as the Local arm ) in this longitude range. We select the 1 Gyr stellar population from the HR diagram in near-infrared, to minimize the dust extinction. We cross-matched Gaia DR2 with the 2MASS PSC (Skrutskie et al. 2006), using the official Gaia DR2-2MASS cross-match best neighbor table (Marrese et al. 2018). For the 2MASS PSC (Skrutskie et al. 2006) we select the sample whose near-infrared photometric quality flag of K s band is at least "A", which means scan signal to noise ratio greater than 10. Bennett & Bovy (2019) argues that the Gaia DR2-2MASS cross-matched sample is complete within 7 < G < 17 mag with conservative estimates. Following their approach, we select the Gaia DR2 sample within 7 < G < 17 mag. The total number of this sample is 39,253,853 (Gaia DR2-2MASS sample).
From the Gaia DR2-2MASS sample, we further select stars whose accurate measurement of the parallax is available in Gaia DR2 (Gaia Collaboration et al. 2018) with a relative parallax uncertainty of π/σ π > 5 (where π and σ π are the parallax and its uncertainty, respectively). Because we are interested in the surface density of the disk stars, we select stars within |z| < 0.3 kpc, where |z| is defined as a vertical position with respect to the Sun's vertical position, z . When we evaluate |z|, we simply assume d = 1/π without taking into account the uncertainty in parallax. To estimate the threedimensional Galactic dust extinction correction, we employed MWDUST 1 (Bovy et al. 2016). This allows us to obtain extinction corrected color, (J − K s ) 0 , and absolute magnitude, M Ks , i.e. the HR diagram as shown in Figure 1.
We then select the stars within 0.1 ≤ (J − K s ) 0 ≤ 0.2 and 0.0 ≤ M Ks ≤ 0.3 in the HR diagram as our sample for 1 Gyr stellar population, which leaves 33,718 stars. This region in the HR diagram corresponds to the box area highlighted in Figure 1. Figure 1 also shows the track of PARSEC+COLIBRI isochrones (Bressan et al. 2012;Marigo et al. 2017) with ages of 1 and 1.5 Gyr with the solar metallicity (Z = 0.0152) and a lower metallicity of Z = 0.0096. The figure indicates that our selected region in the HR diagram corresponds to turnoff stars whose age is between about 1 and 1.5 Gyr with the metallicity expected in the disk stars outside of the solar radius, where we focus on in this paper. There could be some contamination of blue horizontal branch stars of the Galactic halo stars in this color and magnitude range. We analyzed the vertical distribution of our selected stars, and confirmed that they are mostly confined within |z| < 0.2 kpc. We also confirmed the stellar density drops rapidly with |z|. Hence, we consider that in the volume we study in this paper the thin disk stars are dominant, and the contamination of blue horizontal branch stars is negligible.
We found that our sample is estimated to be complete in an acceptably high level within 0.2 ≤ d ≤ 1.33 kpc. This corresponds to the projected distance in the disk plane, d xy , of 0.2 < d xy < 1.3 kpc, when the sample is limited within |z| < 0.3 kpc as mentioned above. We exclude the stars within d xy < 0.2 kpc, because Gaia DR2 is incomplete for nearby bright stars with G < 7 mag. We also exclude the stars at d xy > 1.3 kpc, because the completeness drops at the farther distance. Hence, for our sample after cross-matching Gaia DR2 and 2MASS data. The bin size is 0.1 × 0.1 mag and the color indicates number of stars per bin as shown with the color bar at the right. The left and right magenta (black dashed) lines indicate the PARSEC+COLIBRI isochrone with an age of 1 and 1.5 Gyr, respectively, with the solar metallicity (a metallicity of Z = 0.0096). The solid box represents the color-magnitude ranges for selecting our 1 Gyr age population.
our final sample used in this paper is limited within 0.2 < d xy < 1.3 kpc and |z| < 0.3 kpc. This leaves our final sample of 4,654 stars.
We evaluated that our sample is complete in an acceptably high level within the distance (d) between 0.2 and 1.33 kpc as follows. Figure 2 shows the extinction, A Ks , in our selected Galactic longitude region, i.e. 90 • ≤ l ≤ 270 • , within |z| < 0.3 kpc from the Sun and the distance within 0.2 ≤ d ≤ 1.33 kpc, using MWDUST. We found that almost all the sample have A Ks < 0.6 mag. Then, our sampled absolute magnitude range of 0.0 ≤ M Ks ≤ 0.3 mag corresponds to 6.5 ≤ K s ≤ 11.5 mag at 0.2 ≤ d ≤ 1.33 kpc with the maximum extinction of A Ks < 0.6 mag. The brightest limit of 6.5 mag corresponds to the apparent magnitude of M Ks = 0 mag at the minimum distance of d = 0.2 kpc and the faintest limit corresponds to the apparent magnitude of M Ks = 0.3 mag at d = 1.33 kpc plus the maximum extinction of A Ks = 0.6 mag. We found that our sample within the square region of Figure 1, i.e. 0.1 ≤ (J − K s ) 0 ≤ 0.2 mag and 0.0 ≤ M Ks ≤ 0.3 mag, are within 0.5 < G − K s < 5.5. This means that for our sample 6.5 ≤ K s ≤ 11.5 mag corresponds to 7 < G < 17 mag. As discussed above, according to Bennett & Bovy (2019) that Gaia DR2−2MASS crossmatched sample is complete within 7 < G < 17 mag.
However, our final sample is additionally limited to the stars with π/σ π > 5. Hence, we compare our final sample with the Gaia DR2-2MASS sample in our selected volume and color-magnitude range. To this end, we made a comparison sample, Group C, from the Gaia DR2-2MASS sample, which has 7 < G < 17 mag cut, by selecting the stars within 0.1 ≤ (J − K s ) 0 ≤ 0.2 mag, 0.0 ≤ M Ks ≤ 0.3 mag, |z| < 0.3 kpc and 0.2 < d xy < 1.33 kpc, using their distance of d = 1/π, regardless of their uncertainty. Parallax uncertainties of Group C can be large. Therefore, there are contamination from the stars whose true distance, their absolute magnitude or color is not within the selected range. Also, Group C must be missing some stars whose true distance, color and magnitude are within the selected range of our final sample, but not in Group C, because of their error in parallax. Here, we consider that these can compensate each other in some degree, and Group C is close to being a reasonable representative complete sample to be compared with our final sample for simplicity. We obtain 4,798 stars in Group C and 4,654stars satisfy π/σ π > 5. This leads to 97% stars in Group C being in our final sample, and the additional cut of π/σ π > 5 does not reduce the sample fraction significantly. Hence, our final sample is considered to be a reasonably representative sample to estimate the density distribution of our selected population of stars.
Note that here we used the cataloged values of parallax, color and magnitude in Gaia DR2 and 2MASS without taking into account the uncertainty. In addition, 3D dust extinction is still uncertain even in this area of relatively near the Sun, but we simply use mwdust to correct the dust extinction, for simplicity. These errors in these measurements and uncertainties in the dust extinction affect which stars are included in our color-magnitude range or within the chosen spatial range of distance and the height. In this paper, we assume that these errors affect in both ways in increasing and decreasing the sample compared to the true sample. These compensate each other, and the final results are less affected by these uncertainties. Still, more statistical test is required to properly assess the effects of these errors. We postpone such statistical study to a future paper, but this paper provides more qualitative indications from the selected sample which are chosen to be a representative sample for our selected stellar population.

High Mass Star Forming Regions and the Local arm
As discussed in Section 1, the Local arm is currently identified by the star forming regions, young OB stars and young open clusters (e.g., Xu et al. 2018b). To define the location of the Local arm where the stars are forming, we use HMSFRs as shown in Xu et al. (2016), to compare the stellar density distribution from our selected Gaia DR2 stars in the previous section. To define the location of the Local arm from the star forming regions, using the model described in , we fit the distribution of HMSFRs with a following logarithmic spiral-arm model, where R ref is a reference Galactocentric radius, β ref is a reference azimuthal angle and ψ is a pitch angle. The zero point of the Galactocentric azimuthal angle, β, is defined as a line toward the Sun from the Galactic center and the angle increases toward the direction of the Galactic rotation. β ref was set near the midpoint of the azimuthal angles for the Local arm HMSFR sources in Xu et al. (2016). Because in this paper we focus on the stellar density distribution in the second and third Galactic quadrants (90 • ≤ l ≤ 270 • ), we apply the fitting with equation (1) to the 12 Local arm HMSFR sources within 90 • ≤ l ≤ 270 • . Then, we obtained (R ref , β ref ) = (8.87 ±0.13 kpc, 1.4 • ) and ψ = 13.1 • ±7.5 • . The arm's width, a w , defined as the 1σ scatter in the sources perpendicu-lar to the fitted arm position, is 0.19 kpc. The location of the Local arm identified with HMSFRs (HMSFRsdefined Local arm, hereafter) is shown with the solid line in Figure 3, and the dashed lines show the width of the arm. Note that two HMSFRs are outside of the region shown in Figure 3, where only 10 HMSFRs are seen. Also note that this location of the HMSFRsdefined Local arm is different and has a significantly larger pitch angle than the Local-arm identified in Xu et al. (2016), because Xu et al. (2016) included the Local arm HMSFRs sources in the lower Galactic longitude, 70 • ≤ l ≤ 270 • . Our result provide better fit in the region where we are interested in this paper. The spiral arm may be segmented and different part of the arm may have different pitch angles (e.g. Honig & Reid 2015). Therefore, we use our new fit of the HMSFRsdefined Local arm in the region of our interest in this paper. Xu et al. (2016Xu et al. ( , 2018a identified a minor segment situated between the Local and the Sagittarius arms in the first quadrant. We confirmed that the extrapolation of the minor segment does not come close to the HMSFRs-defined Local arm. Hence, we do not consider the minor segment is related to the HMSFRs-defined Local arm in the region we focus in this paper.

RESULTS
Using the sample of stars selected as 1 Gyr old population as described in Section 2.1, we analyzed the surface density distribution of 1 Gyr old stars. The smoothed surface density distribution is shown in the left panel of Figure 3. Here, we define x-axis as a direction of the rotation from the Sun with the Sun's location at x = 0 kpc, and the y-axis is the direction from the Galactic center to the Sun whose location is y = r 0 = 8.34 kpc. The red inner and outer dashed half-circles indicate the distance from the Sun of d xy = 0.2 and 1.3 kpc, respectively. As discussed in Section 2.1, the completeness of our sample drops rapidly inside of the inner red dashed circle or outside of the outer red dashed circle. Hence, we trust the density map only between these two red dashed half-circles. The solid line shows the location of the Local arm defined with the HMSFRs-defined Local arm in Section 2.2. Interestingly, there is a clear stellar overdensity of the 1 Gyr old stars at a similar location to the HMSFRs-defined Local arm at 90 • ≤ l ≤ 190 • , or slightly outside of the HMSFRs-defined Local arm at a larger Galactic longitude at l ≥ 130 • . The most significant stellar overdensity is seen between l = 90 • and l = 110 • . The stellar overdensity looks extended along the HMSFRs-defined Local arm from l = 90 • to l = 190 • at least. In the region of the larger Galactic longitude than l = 190 • , although there are HMSFRs, and the HMSFRs-defined Local arms extends continuously as shown in the black solid line and the dashed lines, the extension of the stellar overdensity is not clear within our distance limit.
To take into account the mean stellar density decrease with the increasing Galactocentric radius, the right panel of Figure 3 shows the smoothed density distribution of 1 Gyr stars after divided by an exponential density profile with the scale length of r d = 2.5 kpc (e.g., Bland-Hawthorn & Gerhard 2016). The arm-like structure of the stellar overdensity in 90 • ≤ l ≤ 190 • as seen in the left panel of Figure 3 still exists after taking into account the decrease in the stellar density at the outer radii.
To quantify the significance of this overdensity, we compute the stellar density after divided by the exponential law as a function of the distance from the Sun in the different longitudinal regions between l = 90 • and l = 210 • . The results are shown in Figure 4. We evaluated the uncertainty of the density in each distance bin by taking the dispersion of the density in each bin measured from 500 bootstrap realization of the sample. Within 90 • ≤ l ≤ 110 • the stellar density increases with the distance from the Sun, and the density peak is seen at close to our distance limit of d xy = 1.3 kpc, as seen in Figure 3. Although it is not very clear at 110 • ≤ l ≤ 130 • , at 130 • ≤ l ≤ 190 • , we can see a more clear peak of density within our distance limit, and the density decreases with the increasing distance after passing the density peak. This peak corresponds to the arm-like overdensity seen in Figure 3, and the significance of the overdensity is about 2σ, when comparing the highest density peak and the uncertainty especially at 130 • ≤ l ≤ 170 • . Hence, we think that the stellar overdensity seen in Figure 3 is very likely a real structure. Figure 4 also confirms that at l ≥ 190 • the overdensity is not very clear. The histograms of the density distribution as a function of distance in 190 • ≤ l ≤ 210 • show a hint of the overdensity, but it is not statistically significant. Hence, as seen in Figure 3, at l ≥ 190 • there is no significant stellar component corresponds to the HMSFRs-defined Local arm or they are farther than the distance we can confidently analyze the stellar density.
The vertical grey area in Fig. 4 shows the distance range of the HMSFRs-defined Local arm in the corresponding Galactic longitude range in each panel. Interestingly, at 130 • ≤ l ≤ 190 • the location of the stellar Local arm overdensity is slightly outside of the HMSFRs-defined Local arm at a larger Galactic longitude. On the other hand, at lower Galactic longitude, 110 • ≤ l ≤ 130 • the HMSFRs-defined local arm is located at the center of the stellar overdensity, although the width of the arm overdensity is not very clear. This trend is also seen in the right panel of Figure 3. If this is true, the stellar Local arm we identified has a slightly larger pitch angle than the HMSFRs-defined Local arm. We will discuss the implication of this result in Section 4.

SUMMARY AND DISCUSSION
Taking advantage of the precise measurements of parallax for a large number of stars recently provided by Gaia DR2, we analyzed surface stellar density map for a relatively old (∼ 1 Gyr) stellar populations of the thin disk stars between 90 • ≤ l ≤ 270 • . We identified the 1 Gyr population from a carefully chosen range of the color and magnitude in the near-infrared bands, after cross-matching Gaia DR2 and 2MASS. We evaluated that our sample is reasonably complete within the distance between 0.2 and 1.3 kpc. We found a marginally significant arm-like stellar overdensity close to the Local arm identified with the HMSFRs especially in the region of 90 • ≤ l ≤ 190 • . At l ≥ 190 • we could not find a significant stellar overdensity. At 90 • ≤ l ≤ 190 • the identified stellar Local arm is located similar region to the HMSFRs-defined Local arm. Our finding indicates that the Local arm is not a minor arm with only the gas and star forming clouds, but a significant stellar overdensity is associated, too.
Interestingly, at 130 • ≤ l ≤ 190 • the identified stellar Local arm is located slightly outside of the HMSFRsdefined Local arm, while at lower Galactic longitude of 90 • ≤ l ≤ 130 • the stellar Local arm is co-located with the HMSFRs-defined Local arm. This indicates that the pitch angle of the stellar arm is slightly larger than the HMSFRs-defined arm, and there is an offset between HMSFRs-defined (i.e. gas) and stellar arms especially at the larger Galactic longitude, 130 • ≤ l ≤ 190 • . The offset and different pitch angles between the stellar and gas spiral arms are consistent with what is expected from a classical density-wave and its galactic shock theory (e.g., Roberts 1969). Hydrodynamic simulations with the rigidly rotating spiral arm potentials also consistently show that the pitch angle of the gas arm is smaller than that of the (stellar) spiral arm (Gittins & Clarke 2004;Baba et al. 2015). However, we note that the pitch angle of the stellar Local arm is larger compared to the other major spiral arms like the Perseus arm and the Scutum-Centaurus arm (e.g. ). This could be an issue for a classical density-wave theory where a constant pitch angle is expected in the different spiral arms at least at the same radius. More complicatedly, Vallée (2018) found an offset between the CO  arm and the HMSFRs-defined arm in the Perseus arm, where the CO spiral arm (earlier phase of gas spiral arm) shows a larger pitch angle than the HMSFRs-defined spiral arm. How this can be compared with the offset between the stellar arm and the HMSFRs-defined arm is not a trivial question and Pour-Imani et al. (2016) argues that there are two scenarios of the offset of stellar and gas spiral arms in the density-wave scenario. It is required to further study the offset between different arm tracers in the different spiral arms in the Milky Way. More clear theoretical predictions in the density-wave scenario are also necessary.
In Figure 3, we also show the locations of the H II regions from Foster & Brunt (2015) who measured the distance to the H II regions within 90 • ≤ l ≤ 190 • . The H II regions are also located in the similar region to the stellar overdensity we identified. Interestingly, the right panel of Figure 3, which shows the stellar overdensity after taking into account the mean stellar density decrease with the increasing Galactocentric radius, tentatively shows that the H II regions seem to be located between the identified stellar arm and the HMSFRsdefined Local arm. Admittedly, this is a quite tentative trend with very low number statistics. However, if this is confirmed, because the H II regions are considered to be the star formation tracer phase later than HMS-FRs, the offset between HMSFRs, the H II regions and the stellar arm would provide the strong support for the density-wave scenario. Lépine et al. (2017) suggested that the Local arm is caused by the trapped orbits at the co-rotation resonance of the major spiral arms of the Perseus and the Sagittarius-Carina arms. Our stellar overdensity in the similar location to the Local arm traced by HMSFRs and H II regions does not contradict with this scenario. However, if the offset between these different populations is confirmed to be true, this scenario may be difficult to explain such offset and different pitch angles for different populations. The stellar Local arm identified in this paper encourages further quantitative comparison between the model and the observed features.
The offset between the gas and stellar arms is also difficult to be explained with the dynamic spiral arm scenario, where no "systematic" offset between the stellar and star forming arms are expected (Grand et al. 2012a;Baba et al. 2015). On the other hand, the large pitch angle of the Local arm is consistent with the currently forming spiral arm for the dynamic spiral arm scenario (Baba et al. 2013;Grand et al. 2013). Also, the recent observations of the converging velocity field around the Local arm (Liu et al. 2017) is consistent with the ongoing formation of the Local arm. This converging velocity field is different from the diverging velocity field observed around the Perseus arm Tchernyshyov et al. 2018). The dynamic spiral arm scenario can explain these differences in the velocity field and pitch angles between the Perseus arm and the Local arm, if the Perseus arm is in a disrupting phase, while  The stellar density contrast shown in these panels are the surface density of our sample after divided by an exponential profile as the right panel of Fig. 3. The vertical error bars show the uncertainties evaluated by 500 bootstrap sampling. The vertical grey area indicates the distance range of the HMSFRs-defined Local arm as highlighted with the solid black line in Figure 3 in the corresponding Galactic longitude ranges.
the Local arm is in a building up phase (Baba et al. 2013;Grand et al. 2014;Baba et al. 2018). However, the dynamic spiral arm scenario has to be able to explain the significant offset found in this paper. The significant external perturbation (but see also Michtchenko et al. 2019, for an alternative scenario), which is suggested to explain the Galactic disk in-plane and vertical motions found in Gaia DR2 Antoja et al. 2018;Bland-Hawthorn et al. 2019), may affect the origin of the spiral arm in the Milky Way (Laporte et al. 2018), and may be able to explain this offset. Further modelling of the spiral arms including the external perturbations of the Galactic disk is necessary to further understand the formation mechanism of the spiral arm.
Unfortunately, the edge of the stellar Local spiral arm is close to our distance limit. Also, although we carefully take into account the completeness of the Gaia DR2 data, further studies with better data and also taking into account the selection function (e.g. Bovy 2017) are required to accurately map the Local arm and the other spiral arm at the farther distances, and answer this long-standing challenge of understanding the origin of the spiral arms in the Milky Way. The result of this paper provides a new and complex picture of the Local arm, and encourages such further work. The expected parallax accuracy for the fainter stars in the next Gaia data releases will certainly help, to map the stellar density structures for the different age populations. Ultimately the near-infrared astrometry mission like the small-JASMINE (Gouda 2012) and ultimately the mission like Gaia NIR concept (Hobbs et al. 2016) would be required to answer the structure and origin of the spiral arms.
We are grateful to the anonymous referee for constructive comments that have improved the paper. We acknowledge Dr. Mark J. Reid for allowing us to use his MCMC program, utilized to define a locus of the Local spiral-arm, traced by HMSFRs. DK thanks the generous support and hospitality of the National Astronomical Observatory of Japan and the Kavli Institute for Theoretical Physics (KITP) in Santa Barbara during the 'Dynamical Models For Stars and Gas in Galaxies in the Gaia Era' program. KITP is supported in part by the National Science Foundation under Grant No. NSF PHY-1748958. DK also acknowledges the support of the UK's Science & Technology Facilities Council (STFC Grant ST/N000811/1). JB is supported by the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Scientific Research (C) Grant Number 18K03711. NM and JB are supported by the JSPS Grant-in-Aid for Scientific Research (B) Grant Number 18H01248. Data analysis was carried out on the Multi-wavelength Data Analysis System operated by the Astronomy Data Center (ADC), National Astronomical Observatory of Japan. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/ consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. 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. We are indebted to NASA's ADS for its magnificent literature and bibliography serving.