Wavelet analysis is performed at each pixel location of SJ FOV to obtain the period of SJ intensity variability over the observed moss region. As shown in Figure 1, a typical light curve corresponding to a single pixel location for the entire duration reveals presence of quasi-periodic small and large amplitude intensity fluctuations. Figure 2A shows a representative example (selected at random) of wavelet analysis results corresponding to the pixel location marked as A in SJ FOV (Figure 1) for a duration of 20 min. It should be noted that in most of results we show the wavelet and EMD analysis corresponding to 20 min interval only so that the temporal variations in intensity can be studied more carefully, particularly as we are interested in the shorter periodicities. The top panel in Figure 2A shows the variation of SJ intensity with time. The middle-panel shows the background (trend) subtracted intensity which is further used to obtain wavelet power spectrum (lower panels). The background (trend) is obtained by taking the 10-point running average of the intensity variation. The bottom left panel displays a wavelet power spectrum (color inverted) with 99% significance levels and the bottom right panel displays a global wavelet power spectrum (wavelet power spectrum summed over time) with 99% global significance.

The power spectra obtained reveals the presence of short-period variability in the SJ intensity light-curve, with a distinct power peak at a period of 1.6 min. It is important to note that even without considering the background trend, we obtain a power peak at the same period in wavelet spectra but with low significance level. Empirical mode decomposition (EMD) is also employed at a few locations in the SJ FOV. Figure 2B shows the different intrinsic mode functions (IMFs) obtained from EMD for the same SJ light-curve as shown in Figure 2A. Here only the first four IMFs are shown as the further IMFs contain the larger background trends. The dominant period (P) mentioned in the figure for each IMF is calculated using fast-Fourier transform (FFT). The period of the first four IMFs for the particular example shown in Figure 2B are 0.74, 1.25, 2.85, and 3.99 min. The EMD analysis reinforces the detection of the presence of short periodicities (1–2 min) in the moss region as obtained by wavelet analysis. The presence of periodicities < 1 min can also be noted from the Figure 2, though these are below the significance level of 99% as shown in wavelet power spectra. Such oscillations have very small amplitudes, are present even for shorter-duration and could be damping fast. Hence, the oscillations with periods < 1 min may carry smaller amount of energy and may not be so important as those with periods > 1 min which may be distributed over larger spatial and temporal extents.

To focus on the distribution of power as calculated from the wavelet method, we obtain the power maps of SJ intensity over the full FOV in 1–2 min and 2–4 min period intervals (Figure 3) by considering the entire duration of the observation. The entire duration of the observations is chosen to understand the global dynamics of the active region moss. On comparison of power maps with the SJ images (Figure 3) and AIA images (Figure 1), it can be observed that the significant power of high-frequency (1–2 min) as well as low-frequency (2–4 min) oscillations is generally present only in bright regions of the moss. Figure 3 also shows the time-average SJI with the power contours of 1–2 min variability in red and 2–4 min in yellow. The power contours enclose the locations with the value of significant power to be more than 100, in respective period range. The finer and smaller spatial extents of the contours at various locations over the field of view suggest that these oscillations possess high power in the localized regions within the bright moss. Moreover, the comparison of power between short (1–2 min) and long (2–4 min) periodicities, as showcased in Figure 3, reveals that the power in 1–2 min variability is, in general, less than that in 2–4 min.

To characterize periodicities present in the spectrograph data, we produce power maps of the spectral parameters obtained by fitting a single Gaussian to the Si IV 1403 Å emission spectra using wavelet analysis. The analysis was performed over the entire duration of the observations. At few instances, we interpolate the spectral parameters where a Gaussian fitting could not be performed due to poor signal to noise. The power maps, shown in Figure 4, clearly showcase the significant power along the slit, predominantly present in the period range of 0.83–2.36 min corresponding to pixel locations of the bright moss regions (wherever the slit crosses the bright moss). This confirms the presence of short-period oscillations in Si IV 1403 Å spectra along with the Si IV 1400 Å SJ intensity (described in section 3.1) in various locations of the moss region.

Now we shift our focus to shorter time intervals where data gaps due to poor signal-to-noise are absent. This allow us to investigate the correlation between different spectral parameters using wavelet and EMD analysis. Further, taking the intervals of 20 min is sufficient because we are primarily interested in shorter periods like, 1–2 min. Figure 5A shows the wavelet maps of total intensity variation for a duration of 20 min at a particular location along the slit (marked as B in the SJ FOV in Figure 1). Total intensity signifies the summed intensity over the wavelength range. Figure 6A shows the wavelet maps of Doppler velocity at the same location B and same time-interval as shown for total intensity in Figure 5. Note that the location B is very close to location A so that a comparison can be made with the periodicities found at location A using SJI. Moreover, the same time-interval is shown in Figures 2, 5, and 6 for better illustration. Figure 7 shows the variation of peak intensity, Doppler width, total intensity and Doppler velocity of Si IV 1403 Å line at location B along with the spectral line-profile at a particular instance. The observational uncertainties are shown in the left panel over the observed line-profile. These errors are taken into account while fitting the Gaussian profile (green solid curve). The fitting errors of the respective spectral parameters are shown in the adjacent light curves in orange. It can be clearly observed that the errors in the spectral parameters are much less than the amplitude of oscillations. For instance, the average magnitude of error over the Doppler velocity light curve shown in Figures 6, 7 is 0.5 km/s, whereas the amplitude of oscillation of its IMFs (as shown in Figure 6) is more than 1 km/s in most of the cases. The oscillations in the spectral parameters are well above the error values in general and thus significant. An animation of the Figure 7 is available as the supplementary material (Supplementary Video 1) in the online version which shows the evolution of the spectral line profile with time.

The background trends for the spectral parameter light curves (in Figures 5, 6) are obtained by considering the 35-point running average of the light-curves. The dominant power peaks are observed to be present 1.5 min for total intensity, 1.7 min for peak intensity, 1.7 min for Doppler velocity, and 1.5 min for Doppler width in the respective power spectra. Here again, the presence of periodicities of < 1 min can be seen in the wavelet. It can be clearly observed that such oscillations are present for very short durations and thus of not much significance over the longer durations. Also, such short periodicities could be due to the presence of noise which is picked up by wavelet at higher-frequencies.

The EMD technique is applied over the spectral variations in order to segregate the different periodicities present in their light curves. Figures 5B, 6B, respectively, shows the first four IMFs and their periods (P) of total intensity and Doppler velocity variation for the duration of 20 min at the location B. The first four IMFs (IMF0, IMF1, IMF2, and IMF3) are observed to contain the short-period variabilities (0.2–2 min). The successive IMFs are observed to have periodicities of more than 2 min and hence not discussed in the present analysis. To perform a statistical study of correlation and phase-relationship between Doppler velocity and total intensity, we study 40 different light-curves (cases), each of duration 20 min. These cases are selected to be located in the close neighborhood of the power contours of 1–2 min periodicities (red contours in the average SJ image in Figure 3). The locations of the selected cases are marked in black along the slit in the SJ image in Figure 3. Few specific time-intervals are considered at these locations in order to have further study about phase-relationship between Doppler velocity and total intensity.

Figure 8 shows the histograms of the period of oscillations for different IMFs of total intensity and Doppler velocity with the mean periods listed in the figure. As reflected by the value of mean periods, we will further regard the IMF0 to be associated with the periodicity of ~0.17 min, IMF1 with ~0.40 min, IMF2 with ~0.72 min and IMF3 with ~1.26 min. The power maps in Figure 4 shows the absence of significant power in the periods below 0.6 min. Henceforth, for the further analysis about phase-relationship, we consider only the third and fourth IMFs, i.e., IMF2 and IMF3. The phase-relation between Doppler velocity and total intensity at the short-periodicities is studied by correlating their respective IMFs for the 40 cases. Figure 9 shows the histograms of the phase difference between Doppler velocity and total intensity by considering IMF2 and IMF3. The sign convention for the values of phase-shifts considered here is such that the positive values phase-shift signifies the Doppler velocity to be leading with respect to the total intensity. The histogram of IMF2 reveal the presence of preferred phase-shifts at ~ ±3T/8 (~ ±3π/4) where T = 0.72 min, is the time period of oscillation. The histogram of IMF3 shows the dominant phase-shifts at ~ −T/2 (~ −π) where T = 1.26 min.

The presence of a dominant phase shift of ~T/2 for periodicities of ~1.26 min (IMF3) indicates the presence of reconnection events. As shown in Figure 7, the increase in the intensity is accompanied by the increase in the Doppler width and decrease in Doppler velocity (blue-shifted flows, De Pontieu et al., 2009; De Pontieu and McIntosh, 2010) at many instances throughout the light-curve. Few of such instances are shown by vertical dotted lines in Figure 7. In case of phase-shifts of ~±T/2 or ~±π, the reconnection process results in near simultaneous variation in the spectral parameters with the resultant mass flow projected toward the line-of-sight (blue-shifts or negative Doppler velocity). As the TR emission lines are red-shifted in general, the flows toward the line-of-sight (blue-shifted flows) will appear to decrease the Doppler speeds simultaneously with the increase in the intensity and width (phase-shift of ~±T/2 or ~±π). On the other hand, the flows away from the line-of-sight will increase the value of the Doppler speeds with an increase in the line intensity and width (~ zero phase-shift). It can be observed from Figure 7 and also indicated by Figure 9 that the red-shifted flows (cases with zero phase difference) occur less frequently compared to blue-shifted flows (cases with phase shifts of ±T/2). As shown in Figure 7, the instances of large amplitude fluctuations, which mostly have phase shift of ~T/2 between Doppler velocity and total intensity, can be regarded as the clear signatures of quasi-periodic outflows (toward the observer) resulting from the reconnection process. The other instances of small amplitude fluctuations can be due the presence of slow magneto-acoustic waves.

Very recently, Hansteen et al. (2014) and Brooks et al. (2016) have reported the presence of transition region fine loops with the aid of IRIS observations and numerical simulations. Such small scale loops with loop lengths of ~1 to 2 Mm can harbor slow standing waves with periods of ~1 min in transition region. It is worth noting at this point that Wang et al. (2003); Taroyan et al. (2007); Taroyan and Bradshaw (2008) reported the presence of standing slow waves exclusively in hot coronal loops. In addition, Pant et al. (2017) reported the existence of standing slow waves in cool coronal loops (~0.6 MK). In this work, we found evidence of the existence of slow waves in Si IV 1403 Å emission line whose formation temperature is ~60000 K. In an ideal case, the phase-shift of ~±T/4 is attributed to the presence of standing slow waves in the solar atmosphere (Wang et al., 2003; Taroyan et al., 2007; Taroyan and Bradshaw, 2008; Moreels and Van Doorsselaere, 2013). Further, it should be noted that the intensity and velocity changes phase in time due to the heating and cooling of the plasma (Taroyan and Bradshaw, 2008) and due to presence of imperfect waveguides and drivers in reality, which deviates from the theoretical considerations (Keys et al., 2018). Thus the phase shift between intensity and velocity oscillations might differ in different regions and different time as showcased in Figure 10. Figure 10 shows the representative examples of the IMFs (IMF2 and IMF3) at location B along the slit. The phase-shift between Doppler velocity and total intensity (ϕ) obtained using the correlation techniques is also mentioned in the respective panels. The comparison between of the respective IMFs of intensity and Doppler velocity fluctuations clearly depicts that the phase-shift between them changes continuously throughout the entire duration. This could be due to the intermittent nature of the flows and waves that might result in departure from the theoretically expected values of the phase-shifts. Hence we conjecture that the statistically dominant phase shift of ~±3T/8 for periodicities of ~0.72 min (IMF2) is due to the presence of small-scale flows along with slow standing waves in TR fine loops. This supports both wave and reconnection like scenario to be responsible for the periodicities of 1–2 min in moss regions, which is discussed in details in section 4.

In order to obtain the information about density variations associated with the presence of waves and/or reconnection flows, in the moss regions, we attempt to estimate density along the slit using Si IV 1403 Å (λ = 1402.77 Å) and O IV 1401 Å (λ = 1401.16 Å) spectral lines from the IRIS spectra (as suggested by Young et al., 2018). They introduced an empirical correction factor to normalize Si IV/O IV line intensity ratios. As first mentioned by Dupree (1972), the observed intensities of lines from the lithium and sodium-like iso-electronic sequences are usually stronger than that expected by the emission measures from other sequences formed at the same temperature. Hence, such a correction factor is important to be applied to silicon line intensities. Table 2 of Young et al. (2018) gives the theoretical ratios of different lines after employing the correction factor (see QS DEM method as explained in Young, 2018; Young et al., 2018). We use the Si IV (1402.77)/O IV (1401.16) line ratio from Table 2 of Young et al. (2018) for the estimation of electron density at a temperature of logT/K = 4.88 (temperature of maximum ionization of Si IV).

As the O IV 1401 Å line is very weak in IRIS spectra, the spectra is averaged over 7 pixels along the slit. In such averaging, for instance, the data value of the first 7 spatial pixels are replaced by their average value, the next 7 pixels are replaced by their respective average data-value, and so on. Similarly, time-averaging is also performed by considering 4 time steps along the temporal axis. In order to improve S/N, such averaging is performed only over O IV 1401 Å spectra as Si IV 1403 Å spectra contains significantly good signal. Figures 11A,B shows the time-sequence maps of peak intensity along the slit for the Si IV 1403 Å and O IV 1401 Å line-profiles. A comparison between the two maps clearly shows that despite averaging the spectra (as explained above), we are able to obtain good S/N only for very few isolated O IV 1401 Å line-profiles in order to perform a reliable Gaussian fit, hence the peak intensity values for the O IV 1401 Å line are shown only for those isolated few pixels.

Figure 11C shows the theoretical Si IV (1403)/O IV (1401) ratio-density curve (Young et al., 2018) in solid black and the estimated density values are over-plotted in magenta. The density time-sequence map is also showcased in Figure 11D. Note that we could estimate the density only at very few instances of some of the locations, as limited by the poor signal in O IV 1401 Å spectra. It can be observed in Figure 11D that we cannot find considerable examples of continuous density signal along time for some significant amount of duration over the entire observation. It is completely unreliable to perform any time series analysis over such light-curves. It appears that there are definite changes in the density but to relate those changes with intensity and other line parameters for identification of the wave mode is beyond the quality of the current observations. Thus, we are still unable to obtain any results related to density oscillations with the present data.

The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest. The reviewer KS declared a past co-authorship with one of the authors TVD to the handling editor.