2.1. Interferometric fringes

The image plane response of a single interferometer (visibility measured on one baseline) corresponding to the correlator output or spatial coherence, is called a ‘fringe’, which for the general corrupted form is

(6) \begin{align} \widetilde{F}_{ab}(\hat{{\boldsymbol{{s}}}},\lambda) &= \left|\widetilde{V}_{ab}(\lambda)\right| \, e^{i \left[2\unicode{x03C0} {\boldsymbol{{u}}}_{ab}\cdot \hat{{\boldsymbol{{s}}}} + {\unicode{x03C6}}_{ab}(\lambda) + \xi_b(\lambda)-\xi_a(\lambda)\right]}\end{align}

with $\arg \widetilde{F}_{ab}(\hat{{\boldsymbol{{s}}}},\lambda) = 2\unicode{x03C0} {\boldsymbol{{u}}}_{ab}\cdot \hat{{\boldsymbol{{s}}}} + {\unicode{x03C6}}_{ab}(\lambda) + \xi_b(\lambda)-\xi_a(\lambda)\,$ . Ideally, $\arg \widetilde{F}_{ab}(\hat{{\boldsymbol{{s}}}},\lambda)=\arg F_{ab}(\hat{{\boldsymbol{{s}}}},\lambda) = 2\unicode{x03C0} {\boldsymbol{{u}}}_{ab}\cdot \hat{{\boldsymbol{{s}}}} + {\unicode{x03C6}}_{ab}(\lambda)$ occurs when all elements are perfectly phase-calibrated, that is, $\xi_a(\lambda)=0$ for all a.

These fringes are periodic, marked by ‘ridges’ corresponding to where $\arg \widetilde{F}_{ab}(\hat{{\boldsymbol{{s}}}},\lambda)$ is an integer multiple of $2\unicode{x03C0}$ and are given by the null-valued (or zero-valued) isophase contoursFootnote a (and their equivalents offset by multiples of $2\unicode{x03C0}$ ). These are, hereafter, called the fringe null phase curves (NPCs):

(7) \begin{align} 2\unicode{x03C0} {\boldsymbol{{u}}}_{ab}\cdot \hat{{\boldsymbol{{s}}}} + \widetilde{\unicode{x03C8}}_{ab}(\lambda) &= 0 \, , \quad a,b=0,\ldots N-1 \, , \, \textrm{with}\, a\ne b \, ,\end{align}

where, $\widetilde{\unicode{x03C8}}_{ab}(\lambda) = \widetilde{{\unicode{x03C6}}}_{ab}(\lambda) + 2\unicode{x03C0} n_{ab}\,$ , and $n_{ab}$ (an integer) accounts for the NPC offset from the principal NPC ( $n_{ab}=0$ ) by integer multiples ( $n_{ab}$ ) of $2\unicode{x03C0}$ . When traversing anywhere on an NPC (ridge), $\arg \widetilde{F}_{ab}(\hat{{\boldsymbol{{s}}}},\lambda)$ remains unchanged.

The signed positional offset, $\delta s_{ab}(\lambda)$ , of the fringe NPC from the phase centre (origin) along a perpendicular and the corresponding phase offset, $\widetilde{\unicode{x03C8}}_{ab}(\lambda)$ , are related by

(8) \begin{align} \widetilde{\unicode{x03C8}}_{ab}(\lambda) &= 2\unicode{x03C0} \left|{\boldsymbol{{u}}}_{ab}\right|\,\delta s_{ab}(\lambda) \, .\end{align}

Here, $|{\boldsymbol{{u}}}_{ab}|=\left(u_{ab}^2+v_{ab}^2\right)^{1/2}$ denotes the baseline lengths in the projected plane whose normal is the direction to the phase centre. Because ${\boldsymbol{{u}}}_{ab}$ is the spatial frequency of a fringe, $1/|{\boldsymbol{{u}}}_{ab}|$ represents the spatial period of the periodic ridges (or the fringe spacing) in the image plane and corresponds to a phase change of $2\unicode{x03C0}$ , as verified by setting $\delta s_{ab}(\lambda)=1/|{\boldsymbol{{u}}}_{ab}|$ in Equation (8).

Figure 2 shows the ideal fringes, $F_{ab}(\hat{{\boldsymbol{{s}}}},\lambda)$ , in the image plane in direction-cosine coordinates, ( $\ell, m$ ), given by Equation (6) for the modelled 3-element array and the corresponding visibilities shown in Figure 1. The $+$ symbol marks the phase centre (origin). The fringe NPCs, described by Equation (7), are shown in line styles corresponding to those in Figure 1. The black line in each panel denotes the principal NPC ( $n_{ab}=0$ ) of the corresponding fringe. The various grey lines denote the secondary NPCs ( $|n_{ab}|>0$ ) of the fringes. The positional offset, $\delta s_{ab}(\lambda)$ , of the principal fringe NPC from the phase centre is shown by the magenta segments and corresponds to ${\unicode{x03C6}}_{ab}(\lambda)$ (the principal visibility phase) according to Equation (8). In the case of uncalibrated or imperfectly calibrated visibilities, these phase offsets also include the corruptions, $\xi_b(\lambda)-\xi_a(\lambda)$ , arising from the complex gains of the array elements.

Figure 2.

Ideal fringes, $F_{ab}(\hat{{\boldsymbol{{s}}}},\lambda)$ , and the respective NPCs (lines) in the image plane in direction-cosine ( $\ell, m$ ) coordinates, with the line style in each panel corresponding to that of the array element spacings, ${\boldsymbol{{u}}}_{ab}$ , in Figure 1. Equation (7) yields the fringe NPCs. The black lines in each line style corresponds to the principal fringe NPC ( $n_{ab}=0$ ), while the varying shades of grey correspond to secondary ( $|n_{ab}|>0$ ) fringe NPCs. The phase centre (origin) is marked (with a $+$ symbol). The positional offset from the phase centre to each of the principal fringe NPCs is shown in magenta and is related to the visibility phase, ${\unicode{x03C6}}_{ab}(\lambda)$ , by Equation (8).

2.2. Interferometric closure phase

Hereafter, we will assume that the angular power patterns, $\Theta(\hat{{\boldsymbol{{s}}}},\lambda)$ , of the array elements are identical. Consider N elements forming an N-vertex polygon in the aperture plane. The element spacings in the adjacent sides in the polygon are given by ${\boldsymbol{{x}}}_{a\lceil a+1\rfloor_N} \equiv {\boldsymbol{{x}}}_{\lceil a+1\rfloor_N} - {\boldsymbol{{x}}}_a$ , where, $\lceil a\rfloor_N \equiv a \mod N$ . The condition for a closed loop in the aperture plane is

(9) \begin{align} \sum_{a=0}^{N-1} {\boldsymbol{{u}}}_{a\lceil a+1\rfloor_N} &\equiv {\textbf{0}} \, .\end{align}

The interferometric closure phase on the N-polygon is

(10) \begin{align} \widetilde{{\unicode{x03C6}}}_N(\lambda) &\equiv \arg\prod_{a=0}^{N-1} \widetilde{V}_{a\lceil a+1\rfloor_N}(\lambda) = \sum_{a=0}^{N-1} \arg\widetilde{V}_{a\lceil a+1\rfloor_N}(\lambda) \, .\end{align}

Because $\sum_{a=0}^{N-1} \arg G_a^\star(\lambda) \, G_{\lceil a+1\rfloor_N}(\lambda) \equiv 0\,$ ,

(11) \begin{align} \widetilde{{\unicode{x03C6}}}_N(\lambda) &= {\unicode{x03C6}}_N(\lambda) = \sum_{a=0}^{N-1} \arg V_{a\lceil a+1\rfloor_N}(\lambda) \, ,\end{align}

where, ${\unicode{x03C6}}_N(\lambda)$ is the true closure phase on the N-polygon. Therefore, the closure phase is invariant to element-based corruptions, $G_a(\lambda)$ , the corrections from calibration, as well as the errors therein, making it a true observable physical property of the structures in the image plane intensity distribution. This property is a form of gauge-invariance with respect to any element-based phases acquired during the measurement process (Samuel et al. Reference Samuel, Nityananda and Thyagarajan2021; Thyagarajan et al. Reference Thyagarajan, Nityananda and Samuel2021).

A direct consequence of this gauge-invariance is that the closure phase is also invariant to translation in the image plane. This can be shown by replacing $\hat{{\boldsymbol{{s}}}}$ with $\hat{{\boldsymbol{{s}}}}^\prime = \hat{{\boldsymbol{{s}}}} - \hat{{\boldsymbol{{s}}}}_0$ , where $\hat{{\boldsymbol{{s}}}}_0$ is an arbitrary choice for the origin of the image plane, referred to as the phase centre in interferometry. From Equation (2), such a translation modifies the spatial coherence as

(12) \begin{align} V_{ab}^\prime(\lambda) &= e^{i 2\unicode{x03C0} {\boldsymbol{{u}}}_{ab}\cdot \hat{{\boldsymbol{{s}}}}_0}\, V_{ab}(\lambda) \, , \end{align}

which simply introduces an additional phase factor, $e^{i 2\unicode{x03C0} {\boldsymbol{{u}}}_{ab}\cdot \hat{{\boldsymbol{{s}}}}_0}$ , that is factorisable into element-based phase factors, $e^{i 2\unicode{x03C0}{\boldsymbol{{x}}}_b\cdot \hat{{\boldsymbol{{s}}}}_0 /\lambda}$ and $e^{-i 2\unicode{x03C0}{\boldsymbol{{x}}}_a\cdot \hat{{\boldsymbol{{s}}}}_0 /\lambda}$ . Due to the gauge-invariance discussed above, the closure phase is therefore independent of the phase factors introduced by translation in the image plane. Conversely, the translation invariance of the closure phase is simply a special case of the gauge-invariance to the phase factors attributable locally to the array elements.

Because closure phases are unaffected by the corrupting gain terms as is well known and as shown above, without loss of generality, we choose to work with uncorrupted terms in subsequent mathematical analysis unless specified otherwise.

3.1. Relation to the height of the principal triangle

Consider the principal triangle enclosed by the three principal NPCs. The phase centre, $\hat{{\boldsymbol{{s}}}}_0$ , can be conveniently chosen to be at any of the vertices of this triangle, which is the point of intersection of any of the two fringe NPCs, for instance, $F_{01}(\hat{{\boldsymbol{{s}}}},\lambda)$ and $F_{12}(\hat{{\boldsymbol{{s}}}},\lambda)$ . Because $\hat{{\boldsymbol{{s}}}}_0$ lies on the NPCs of both $F_{01}(\hat{{\boldsymbol{{s}}}},\lambda)$ and $F_{12}(\hat{{\boldsymbol{{s}}}},\lambda)$ , by definition, $\delta s_{01}^\prime(\lambda)= \delta s_{12}^\prime(\lambda) = 0\,$ , and therefore, $\unicode{x03C8}_{01}^\prime(\lambda) = \unicode{x03C8}_{12}^\prime(\lambda) = 0$ from Equation (8). Hence,

(17) \begin{align} \unicode{x03C8}_3^\prime(\lambda) &= \unicode{x03C8}_{20}^\prime(\lambda) = \unicode{x03C8}_{20}(\lambda) + 2\unicode{x03C0} {\boldsymbol{{u}}}_{20}\cdot \hat{{\boldsymbol{{s}}}}_0 \nonumber\\ &= \unicode{x03C8}_{20}(\lambda) - 2\unicode{x03C0} ({\boldsymbol{{u}}}_{01}+{\boldsymbol{{u}}}_{12})\cdot \hat{{\boldsymbol{{s}}}}_0 \nonumber\\ &= \sum_{a=0}^2 \unicode{x03C8}_{a\lceil a+1\rfloor_3}(\lambda) = \unicode{x03C8}_3(\lambda) \, .\end{align}

Thus, when the phase centre is chosen to be at any of the vertices of the principal triangle, the closure phase is simply

(18) \begin{align} \unicode{x03C8}_3(\lambda) &= \unicode{x03C8}_{a\lceil a+1\rfloor_3}^\prime(\lambda) = 2\unicode{x03C0} \left|{\boldsymbol{{u}}}_{a\lceil a+1\rfloor_3}\right|\,\delta s_{a\lceil a+1\rfloor_3}^\prime(\lambda)\end{align}

from Equations (8) and (17), where, $\delta s_{a\lceil a+1\rfloor_3}^\prime(\lambda)$ is the height drawn from the vertex chosen as the phase centre, to the opposite side corresponding to the fringe NPC, $F_{a\lceil a+1\rfloor_3}(\hat{{\boldsymbol{{s}}}},\lambda)$ . Thus, the closure phase is directly calculable from a single measurement of any one of the heightsFootnote d of this triangle.

Invariance of closure phase to element-based gain corruptions then implies the heights of the triangle also have to remain invariant. And because the element spacings (baseline vectors) do not change during the measurement process, the orientations of the sides of the triangle in the image plane are fixed. Therefore, all three characteristics, namely, shape, orientation, and size of the triangle in the 3-element interference image are preserved. We will refer to this as the SOS conservation principle. The only remaining degree of freedom for this triangle that does not affect its SOS characteristics is an overall translation.

Figure 3a illustrates these relations geometrically using image obtained by interfering the three fringes, $F_{a\lceil a+1\rfloor_3}(\hat{{\boldsymbol{{s}}}},\lambda)$ , shown in Figure 2. The black and grey lines denote the principal and secondary NPCs of the fringes, respectively, with line styles corresponding to those in Figures 1 and 2. The $+$ symbol marks the phase centre (or the origin) and is denoted by $\mathcal{O}$ in magenta. The principal triangle is shown by the grey shaded region. The positional offsets, $\delta s_{a\lceil a+1\rfloor_3}(\lambda)$ , of the principal fringe NPCs from the phase centre are shown as magenta lines annotated by the corresponding principal visibility phases, ${\unicode{x03C6}}_{a\lceil a+1\rfloor_3}(\lambda)$ , obtained using Equation (8). When the phase centre is conveniently chosen to be at any of the vertices of the triangle (denoted by $\mathcal{O}^\prime$ in red, blue, and brown), the modified visibility phases, ${\unicode{x03C6}}_{a\lceil a+1\rfloor_3}^\prime(\lambda)$ , are proportional to the heights of the triangle, $\delta s_{a\lceil a+1\rfloor_3}^\prime(\lambda)$ , drawn from the chosen vertex (phase centre) shown by the corresponding coloured lines, according to Equation (18).Footnote e The same equation also implies that each of these modified principal visibility phases, ${\unicode{x03C6}}_{a\lceil a+1\rfloor_3}^\prime(\lambda)$ , is equal to the principal closure phase, ${\unicode{x03C6}}_3(\lambda)$ , or in general, $\unicode{x03C8}_3(\lambda) = \unicode{x03C8}_{a\lceil a+1\rfloor_3}^\prime(\lambda), \forall a$ when the $2\unicode{x03C0}$ phase ambiguity (represented by $n_{ab}$ ) is included.

Figure 3b illustrates geometrically the gauge-invariance of the 3-polygon closure phase for uncalibrated (all three element phases corrupted randomly, ranging from 15 $^\circ$ to 75 $^\circ$ ) and translated (in the image plane) fringes in the left and the right panels, respectively, but the discussion applies to both scenarios equally. Both scenarios cause a displacement of the fringes and the NPCs relative to the ideal case in Figure 3a. As a result, the individual principal visibility phases, ${\unicode{x03C6}}_{a\lceil a+1\rfloor_3}(\lambda)$ , relative to the default phase centre, $\mathcal{O}$ , are differently offset relative to the ideal case. However, the closure phase, which is the sum of these three phases remains unchanged as expected. This is also clear geometrically when the phase centre is shifted to any one of the three vertices of the principal triangle (denoted by $\mathcal{O}^\prime$ in red, blue, and brown), the modified phase offset, ${\unicode{x03C6}}_{a\lceil a+1\rfloor_3}^\prime(\lambda)$ , corresponding to the height of the triangle from the chosen vertex to its opposite side, $\delta s_{a\lceil a+1\rfloor_3}^\prime(\lambda)$ given by Equation (18), remains unchanged compared to the ideal case. The fact that the triangle’s heights are unchanged, and the orientations of its sides also remain unchanged because they only depend on the array element spacings, gives rise to the SOS conservation principle. It is important to note that the displacement of the fringes in either case is constrained to be parallel to themselves such that the triangle enclosed by the three vertices of intersection (the grey shaded region), conserves its SOS, and thus the area too, independent of the choice of phase centre. The only degree of freedom for the triangle that does not violate the SOS conservation principle is an overall translation. This is the image plane geometric visualisation of the gauge-invariance of closure phase, and how closure phase is fundamentally related to the properties of the triangle enclosed by the fringe NPCs in the image plane, and not to the phase centre, calibration, or image plane translations. And this is the geometric reaffirmation of the familiar aperture plane view that closure phase is invariant to element-based calibration.

Figure 3.

Illustration of the gauge-invariant and shape-orientation-size (SOS) conserving nature of closure phase. (a) Visibility fringes and phases, and closure phase on ideal (or perfectly calibrated) fringes, $F_{ab}(\hat{{\boldsymbol{{s}}}},\lambda)$ for $a = 0, 1, 2$ , $b = \lceil a+1\rfloor_3$ . The three principal fringe NPCs are annotated and shown in black lines with the line style corresponding to that in Figures 1 and 2 They enclose the principal triangle marked by the grey shaded region. Grey lines denote secondary fringe NPCs. The three principal visibility phases, ${\unicode{x03C6}}_{ab}(\lambda)$ , are proportional to the positional offsets [see Equation (8)] shown in magenta from the phase centre (origin) marked by $+$ and annotated by $\mathcal{O}$ . The closure phase from the principal fringes, ${\unicode{x03C6}}_3(\lambda)$ , is the sum of the three visibility phases. The phase centre can be conveniently shifted to any one of the triangle’s vertices, $\mathcal{O}^\prime$ , marked in brown, blue, or red, in which case the closure phase reduces simply to ${\unicode{x03C6}}_{ab}^\prime(\lambda)$ , which are shown corresponding to the heights drawn from the vertex to the opposite side in brown (dashed), blue (dash-dotted), or red (dotted), respectively, according to Equation (18). Moreover, the area enclosed by the triangle is proportional to the closure phase squared (see Section 3.2). (b) Same as the ideal case in panel (a) but when considering uncalibrated (all three element phases corrupted randomly ranging from 15 $^\circ$ to 75 $^\circ$ ) and translated fringes in the middle and right panels, respectively. As a result, all the fringe NPCs are displaced parallel to themselves relative to the phase centre compared to the ideal case. The closure phase, which is still the sum of the three uncalibrated or translated visibility phases (corresponding to the positional offsets in magenta), remains unchanged. The geometrical equivalence is that the closure phase which is proportional to the heights drawn from one of the triangle’s vertices to the corresponding opposite side (brown dashed, blue dash-dotted, or red dotted lines) are independent of these shifts as well as of the phase centre. Though the individual fringes and the triangle enclosed by them are displaced, their displacements are constrained to be parallel to themselves with the only degree of freedom being an overall translation of the triangle, thereby conserving its SOS characteristics (hence, the area too). The SOS conservation, despite electromagnetic phase corruption attributable to individual array elements, and an overall translation in the image plane, geometrically demonstrates the gauge-invariance of closure phase.

3.2. Relation between areas in aperture and image planes

The closure phase is seen to be intricately linked to the the geometric characteristics of the triangle determined by the fringe NPCs, encapsulated by the SOS conservation principle, which implies that the triangle’s area must also be gauge-invariant. This motivates investigation of the relation between the closure phase and the areas of the triangles enclosed by the fringes and the array elements in the image and aperture planes, respectively. Indeed, it can be shown that

(19) \begin{align} \unicode{x03C8}_3^2(\lambda) &= 16\unicode{x03C0}^2 A_{\mathcal{A}3}(\lambda) \, A_{\mathcal{I}3}(\lambda) \, ,\end{align}

where, $A_{\mathcal{I}3}(\lambda)$ is the area of the triangle enclosed by the three-fringe NPCs in the image plane, $A_{\mathcal{A}3}(\lambda)$ denotes the area of the triangle formed by the locations of the triad of array elements. $A_{\mathcal{A}3}(\lambda)$ is in units of wavelengths squared. The subscripts $\mathcal{I}$ and $\mathcal{A}$ in $A_{\mathcal{A}3}(\lambda)$ $A_{\mathcal{I}3}(\lambda)$ and $A_{\mathcal{A}3}(\lambda)$ denote the image and the aperture plane, respectively, while the subscript 3 denotes a 3-polygon. $A_{\mathcal{I}3}(\lambda)$ is dimensionless as it is obtained using direction-cosine coordinates. See Appendix A for a detailed derivation of this result and associated caveats. A generalisation of these closure phase relationships to a closed N-polygon is provided in Appendix B.

Figure 3 illustrates the quantities in this relationship. $A_{\mathcal{I}3}(\lambda)$ is denoted by the grey shaded area, while $A_{\mathcal{A}3}(\lambda)$ is the area enclosed by the array elements in Figure 1 in wavelength squared units. In this example, $A_{\mathcal{I}3}(\lambda)\approx 1.78\times 10^{-6}$ , $A_{\mathcal{A}3}(\lambda)\approx 34410.43$ , and $\unicode{x03C8}_3(\lambda)\approx -3.11$ radians, thereby validating Equation (19). Thus, using coordinate geometry in the image plane, this work provides a detailed derivation of similar findings from a quantum mechanics perspective (Kobayashi et al. Reference Kobayashi, Tamate, Nakanishi, Sugiyama and Kitano2010).

3.3. A Geometric reasoning for the translation

Here, we provide a geometrical reasoning for the translation of the three-fringe interference pattern in the presence of one or more aperture element-based phase errors. Although fully valid in a radio interferometric context, it is easily described from an optical interferometry viewpoint (see Appendix C).

In the context of aperture masking in optical interferometry, the three aperture elements in Figure 1 correspond to the small unmasked regions of a larger parabolic mirror.Footnote f If we assume beam combination of the type used in most aperture masking experiments, that is, image plane combination where pupil rescaling is the only type of pupil remapping performed, then Figure 2 corresponds to the imaged fringes on the focal plane of the telescope.Footnote g

In this picture, a distortion of the wavefront’s phase at one of the unmasked apertures caused by turbulence in the propagation medium along its path, effectively translates to a simple displacement of the aperture element towards or away from the prime focus, resulting in a net path length or phase difference to the focus. We have shown that such a disturbance will shift the closed three-fringe pattern on the image plane, but will obey SOS conservation. It is easy to see why the three angles of the fringe triangle, and its orientation, are preserved, since these are predetermined by the aperture’s geometry, and thus the fringes can only shift perpendicular to the fringe length, as seen earlier and described by Equations (7) or (13). While less obvious, it remains physically intuitive that the lengths of the triangle’s sides are also preserved, since a phase distortion associated with a single aperture affects the visibilities on the two baseline vectors that include this aperture with equal but opposite values, so that the two fringes involved shift relative to each other in such a way that the lengths between the intersecting vertices are preserved.Footnote h

Figure 4 illustrates the result when the phase of one element in a closed triad is corrupted. The three dark circles indicate the elements (unmasked apertures in an optical telescope, or antennas in a radio interferometer) in the aperture plane (in dark shade of grey), assumed to be on the $Z=0$ plane, whose normal vector is indicated by the thick, solid upward arrow. The radiation is then directed from the elements to the focal (image) plane, wherein a three-fringe image is synthesised by the interference of the EM waves. Consider a phase corruption of one array element (indexed by a) by an amount $\delta\xi_a(\lambda)$ , equivalent to a path length change, $\Delta D_a$ , related by $\delta\xi_a(\lambda)=2\unicode{x03C0}\Delta D_a/\lambda$ , from that aperture element to the focal plane. Since three non-collinear points determine a plane, one can visualise this phase corruption, or the extra path length, at one of the aperture elements as a tilting of the aperture plane relative to the original. The tilted aperture plane and its normal are shown by the light grey-shaded region and the dashed arrow, respectively. Such a tilt then directs the light in a different direction, leading to a shift of the interference pattern in the image plane. Each of the fringes from baselines that contain the phase-corrupted aperture element will be subject to a position offset in the image plane given by Equation (8), $\Delta s_{ab}(\lambda)=\delta\xi_a(\lambda) / (2\unicode{x03C0}\,|{\boldsymbol{{u}}}_{ab}|)$ . Except for the shift, the three-fringe pattern, including the SOS characteristic, is otherwise conserved. These arguments can be generalised to a scenario even when more than one aperture element in a triad is subject to phase corruption.

Figure 4.

A schematic diagram of the effect of a phase error attributable to a single element in a close triad of elements (denoted by dark circles) in an interferometer array. The original aperture plane (in dark grey shade) is at $Z=0$ with normal vector shown by the thick, solid upward arrow, with the focal (image) plane, in the $\hat{{\boldsymbol{{e}}}}_z$ direction. The phase error, $\delta\xi_a(\lambda)$ , at one array element (indexed by a) can be effectively characterised as a change in path length, $\Delta D_a$ , from that array element to the focal plane (sometimes referred to as ‘the piston effect’ Martinache et al. Reference Martinache2020) given by $\delta\xi_a(\lambda) = 2\unicode{x03C0}\Delta D_a/\lambda$ . This change in effective path length leads to a tilt of the aperture plane (in light grey shade) as indicated by the new normal vector (tilted, dashed arrow), and hence a corresponding shift of the image plane. Thus, the image appears displaced relative to the original image plane. The fringes of all baseline vectors that contain the array element with the phase error will each be subject to a position offset as governed by Equation (8), $\Delta s_{ab}(\lambda)=\delta\xi_a(\lambda) / (2\unicode{x03C0}|{\boldsymbol{{u}}}_{ab}|)$ . Regardless of the shift, SOS conservation will apply to the three-fringe interference image.

4.1. Radio quasar 3C 286

The first example is that of radio quasar, 3C 286, which is a bright and highly compact object, often used for flux density and complex bandpass calibration at radio wavelengths. We employ the VLA in its largest (‘A’) configuration and selected three antennas from the array, corresponding to a triangle with projected spacings (baselines) of 12.4, 7.5, and 15.0 km. The flux density of 3C 286 at the observing wavelength of $\lambda=3.2$ cm ( $\nu=9.4$ GHz), measured on these antenna spacings is ${\simeq}4.4$ Jy ( $1\,\textrm{Jy} = 10^{-26} \,\textrm{W}\,\textrm{m}^{-2}\,\textrm{Hz}^{-1}$ ). 3C 286 is the dominant source of emission in the field of view. It has a compact core-jet structure, which on the spatial frequencies being considered herein essentially appears as an unresolved, point-like object (Perley & Butler Reference Perley and Butler2013).

The nearly point-like structure of 3C 286 implies a closure phase very close to zero, which further implies that the three-fringe NPCs will intersect nearly at a point resulting in a nearly degenerate triangle. Equation (18) then implies that the height of such a triangle will be $\delta s_{ab}^\prime(\lambda)\approx 0$ .

We use a short 20 s observation made at $\lambda=3.2$ cm with a narrow bandwidth of 20 MHz. At this wavelength, the spatial frequencies (in units of number of wavelengths) are $|{\boldsymbol{{u}}}_{ab}|=(u_{ab}^2+v_{ab}^2)^{1/2}\approx 3.912\times 10^5$ , ${\approx}2.371\times 10^5$ , and ${\approx}4.749\times 10^5$ , respectively. The root mean square (RMS) level of thermal noise in the calibrated visibilities is ${\approx}33$ mJy, estimated using the VLA exposure calculatorFootnote j using a 2 MHz spectral channel and a 20 s averaging time interval.

We consider both calibrated and uncalibrated data. With the former, the visibilities are expected to add coherently for a sky image, since instrumental and tropospheric phase terms at each element have been determined via a strong celestial calibrator (in this case, 3C 286 itself). The uncalibrated data includes electronics- and troposphere-induced phase offsets for each aperture element in the interferometer array, which need to be corrected via calibration before a coherent image of the target object can be synthesised.

We obtained the interference pattern from a triad of aperture elements as a dirty image (no deconvolution) made from the three visibilities using the task ‘tclean’ of Common Astronomical Software Applications (CASA; McMullin et al. Reference McMullin, Waters, Schiebel, Young, Golap, Shaw, Hill and Bell2007) with zero iterations, which is effectively a sum of the Fourier transforms of the individual visibilities. There are numerous ways in which the fringe NPCs can be geometrically and directly determined from the image plane without recourse to the visibility data in the aperture plane. Here, we employed a simple method, which is neither optimal nor efficient necessarily. In the first step, we determine the intersecting vertices, $(\ell_{a\underline{b}c}, m_{a\underline{b}c})$ , from the interference pattern of any pair of fringes in the image plane, typically using matched filtering followed by peak-fitting algorithm. Of the many possible possible triangles, we preferentially choose the ones closest to the peak of the element power pattern which will yield the best signal-to-noise ratio ( $S/N$ ). Next, given this vertex and the slopes of the two fringe NPCs from the predetermined projected element spacings, ${\boldsymbol{{u}}}_{ab}$ , the individual fringe NPCs that contain this intersecting vertex are determined. Finally, with the three vertices of the principal triangle determined, the closure phase can be measured geometrically using either its height [see Equation (18)] or its area [see Equation (19)].

The thermal noise in the measurements and other systematics will lead to uncertainties in the determined fringe NPCs and thus in the measured closure phase. The phase deviations on the measured visibility phases, $\unicode{x03C8}_{ab}(\lambda)$ , from thermal noise and random systematics in a high- $S/N$ regime ( $S/N\gg 1$ ) follow a Gaussian distribution with a standard deviation that is inversely proportional to the $S/N$ (Taylor et al. Reference Taylor, Carilli and Perley1999; Thompson et al. Reference Thompson, Moran and Swenson2017). The corresponding position error in the fringe NPCs is given by standard error propagation between the pertinent quantities, $\unicode{x03C8}_{ab}(\lambda)$ and $\delta s_{ab}(\lambda)$ , in Equation (8) as

(20) \begin{align} \bigl[\textrm{Var}\left(\delta s_{ab}(\lambda)\right)\bigr]^{1/2} &= \frac{\bigl[\textrm{Var}\left(\unicode{x03C8}_{ab}(\lambda)\right)\bigr]^{1/2}}{2\unicode{x03C0}|{\boldsymbol{{u}}}_{ab}|} \approx \frac{(S/N)^{-1}}{2\unicode{x03C0}|{\boldsymbol{{u}}}_{ab}|} \, .\end{align}

This is also typically the case with astrometric errors in VLBI applications (Thompson et al. Reference Thompson, Moran and Swenson2017). This uncertainty will also propagate into the estimated closure phase. In the 3C 286 data analysed here (2 MHz spectral channel, 20 s integration), the signal strength from 3C 286 and the thermal noise RMS in the visibilities are roughly uniform across the different aperture element spacings giving a $S/N\approx 133$ on each visibility.

Figure 5 shows the three-fringe interference images made from calibrated (left panel) and uncalibrated (middle panel) data. The principal fringe NPCs are shown as black lines (dashed, dot-dashed, and dotted for 12.4, 7.5, and 15.0 km element spacings, respectively). They were determined geometrically using the simple peak-fitting procedure described above and did not use any aperture plane measurements involving the visibilities, except the mathematically predetermined array element spacings, ${\boldsymbol{{u}}}_{ab}$ [see Equation (13)]. For the calibrated data, the fringe NPCs nearly intersect at a point, indeed, on a grid of points, including the position of 3C 286. Importantly, the uncalibrated fringes also result in a similar grid of points. The only change is that the grid shifts by about $.\!\!0^{\prime\prime}2$ relative to the pattern seen in the calibrated data.

Figure 5.

Three-fringe interference images from calibrated (left), uncalibrated (middle), and baseline-dependent phase-corrupted (right) 3C 286 data on projected array element spacings ( $\lambda{\boldsymbol{{u}}}_{ab}$ ) of 7.5 km (dot-dashed), 12.4 km (dashed), and 15 km (dotted) from the VLA. The image coordinates are in Right Ascension (R.A.) and Declination (Dec.) at the J2000 epoch, which are equivalent to the direction-cosine coordinates used earlier (Taylor et al. Reference Taylor, Carilli and Perley1999; Thompson et al. Reference Thompson, Moran and Swenson2017). The principal fringe NPCs (black lines) were determined entirely from the image plane using the method described in the text. The calibrated and uncalibrated three-fringe interference patterns look identical except that the lack of calibration shifts the interference pattern by ${\approx}.\!\!0^{\prime\prime}2$ relative to the calibrated fringes, which indicates the magnitude of the required phase calibration terms. Independent of calibration, the principal fringe NPCs in both cases are nearly coincident with each other which geometrically confirm that 3C 286 has a highly compact structure and the closure phase, ${\unicode{x03C6}}_3(\lambda)\approx 0$ as expected, remains invariant even when the element-based instrumental and tropospheric phase corruption terms remain undetermined. A baseline-dependent phase error (80 $^\circ$ , relative to the calibrated case) on one of the visibilities results in a shifting of the fringes corresponding to that corrupted visibility (from the uncorrupted fringe NPC shown in white dashed line to the corrupted fringe NPC in black dashed line), while the other two remain unchanged. The resulting three-fringe interference pattern (right panel) is very different from the other two panels, and the fringe NPCs are no longer coincident as evident from the non-zero area of the triangle enclosed by the three black lines, and hence, the closure phase is non-zero even for 3C 286, a point-like source. Thus, in the presence of baseline-dependent phase errors, the SOS conservation does not apply to the enclosed triangle, and the three-fringe interference image is no longer a true physical observable.

We also consider a counter-example in the right panel in which an 80 $^\circ$ phase corruption occurs in a visibility in a baseline-dependent manner rather than through one or more individual elements. In this case, two of the fringe NPCs whose visibilities were not corrupted will remain unchanged as they are unaffected by the corruption. Only the fringe NPC of the phase-corrupted baseline will be shifted (uncorrupted in white dashed line and corrupted in black dashed line). This will not result in a change of shape or orientation (which are set by the geometry of the baseline vectors), but will change the size of the triangle enclosed by the three NPCs which effectively modifies the closure phase. And the net three-fringe interference pattern appears to be very different than the calibrated and uncalibrated cases. Therefore, the closure phase (the triangle’s SOS characteristics) will no longer be conserved, implying that the three-fringe interference pattern in the presence of baseline-dependent phase errors is no longer a true physical observable. This demonstrates geometrically that strict closure phase and SOS conservation only occurs if the phase error can be attributed to individual array elements (thereby affecting the visibilities in two baselines with opposite signs), not individual baselines.

The principal closure phases were measured to be ${\unicode{x03C6}}_3(\lambda)\approx 1.7^\circ$ and ${\unicode{x03C6}}_3(\lambda)\approx 2^\circ$ from calibrated and uncalibrated data, respectively. The errors derived from the fitting process, based on Equation (20), are ${\simeq}1.3^\circ$ , implying that both results are indeed statistically consistent with zero closure phase, as expected for a point-like structure.

For verification, it is also possible to calculate the closure phase using the visibilities (in the Fourier- or aperture domain), as is typical in radio interferometry. From the individual visibility phases for each baseline in the triad, we calculate, using Equation (14), a closure phase of $2.6^\circ\pm 0.74^\circ$ and $2.0^\circ \pm 0.74^\circ$ for the calibrated and uncalibrated data, respectively. The RMS uncertainty in the visibility phases was again calculated as a reciprocal of the $S/N$ , in radians. The closure phase is the sum of three visibility phases. Hence, the phase noise, which is uncorrelated between the three visibilities, increases by a factor of ${\simeq}\sqrt{3}$ , to ${\simeq}0.74^\circ$ in the closure phase. These aperture plane estimates of closure phase are statistically consistent with that from the image plane discussed earlier. The quoted uncertainties in the aperture plane measurements represent that expected from thermal noise alone ignoring any potential systematic errors and are thus optimistic relative to the image plane measurements.

This result demonstrates a few important principles. First, the fact that the fringes intersect at a point even for the uncalibrated data geometrically confirms the invariance of closure phase (zero, for a point-like morphology), for an instrument in which the instrumental and tropospheric phase contributions can be factored into element-based terms as in Equation (3). But closure phase is not invariant to baseline-dependent phase errors, which has been shown here geometrically. Second, the shift in the grid pattern in Figure 5 is a measure of the magnitude of element-based phase corruptions due to the instrument and troposphere. Third, the fact that the fringes nearly intersect at a point implies that, for the VLA, the atmospheric and electronic phase corruptions to the data are predominantly factorisable into element-based gains, and are not dominated by corruptions that may be idiosyncratic to a given interferometric baseline. And fourth, it is possible to use this geometric understanding in the image plane for diagnosing baseline-dependent phase errors, provided a model is known for the object being imaged, or in the case of highly redundant arrays. The key distinction between element-based and baseline-based corruptions is that the former will result in an arbitrary translation of fringes in the image plane but conserve the SOS of the triangle, whereas a baseline-based error will fundamentally modify the SOS parameters of the principle triangle, depending on the nature of the baseline-dependent error. For example, a simple baseline-based phase error such as the one discussed above in the 3C286 example will modify only the size of the principal triangle, while a miscalculated antenna spacing vector can modify any or all of the SOS parameters.

4.2. Radio galaxy Cygnus A (3C 405)

As a second example, we employ VLA observations at $\lambda=3.75$ cm ( $\nu=8.0$ GHz) of the bright, extended radio galaxy, Cygnus A (Sebokolodi et al. Reference Sebokolodi2020). Cygnus A has a total flux density of 170 Jy at this wavelength, distributed in two extended lobes with a full extent of $120^{\prime\prime}$ . The observations were made in the ‘D’ configuration of the VLA, which has a longest baseline of ${\approx}1$ km, corresponding to a spatial resolution of ${\approx}8^{\prime\prime}$ . Figure 6 shows an image synthesised from 4 min and 128 MHz of these data. Cygnus A is noted to have complex spatial structure typical of an Fanaroff–Riley II (FR II) morphology (edge-brightened with bright hotspots at the outer edges of their lobes) (Fanaroff & Riley Reference Fanaroff and Riley1974).

Figure 6.

Image of Cygnus A, a bright radio galaxy, synthesised from 4 min and 128 MHz of VLA data at $\lambda=3.75$ cm (Sebokolodi et al. Reference Sebokolodi2020). Cygnus A has a complex structure at these wavelengths: a bright core centred on the active galactic nucleus (AGN) and two bright and non-symmetric lobes, classified as an FR II morphology. The angular resolution of the image (‘beam size’) is ${\approx}8^{\prime\prime}$ . The contours correspond to $-2.5 \sigma$ (dashed), $2.5 \sigma$ , $5 \sigma$ , $10 \sigma$ , $20 \sigma$ , $40 \sigma$ , $80 \sigma$ , $160 \sigma$ , and $320 \sigma$ , where, $\sigma\approx 0.1$ Jy beam-1 is the RMS of noise in the image. The colour bar uses a ‘symmetric’ logarithmic scale to represent both negative and positive values of brightness.

We choose three baselines in a rough equilateral triangle with projected baseline lengths of 797.1, 773.7, and 819.7 m, and respective correlated flux densities of 22.7, 26.4, and 38.3 Jy. We employ a single record with an integration time of 8 s and spectral channel width of 8 MHz, giving a thermal noise of ${\simeq}82$ mJy in a single polarisation.

We employ calibrated data, then corrupt the phase of one of the array elements in a closed triad by 80 $^\circ$ , as would occur if, for instance, there was a significant miscalibration, to detail its geometrical effect on the resulting fringes, and eventually corrupt all three element phases by random amounts ( $-68.4^\circ$ , 101.7 $^\circ$ , and 90.4 $^\circ$ ) as representative of real-world conditions. From the aperture plane visibilities, we calculate a closure phase for the calibrated and the two forms of corrupted visibilities of $112.7^\circ\pm 0.3^\circ$ , where the uncertainty is set by the quadrature sum of the individual phase errors based on the respective visibility $S/N$ ( ${\gtrsim}275$ ) using Equation (20).

In Figure 7, we show the 3-element interference images from calibrated (left panel) and two forms of corrupted data (one element and three element corruptions in the middle and right panels, respectively). In this case, the closure phase is clearly non-zero, and hence the three fringe NPCs do not intersect in a grid of points, as for 3C 286. However, a grid pattern remains visible in the three-fringe images, and this pattern repeats exactly, with a simple shift between the three cases considered. The phase corruption of a single element in the triad as shown in the middle panel is geometrically illustrative. The two fringes involving this corrupted element are shifted, but there is no change in the third fringe. The shifting of the pattern, and thus the triangle enclosed by the fringes, will then occur parallel to the uncorrupted fringe, as indicated by the red double-headed arrow in the middle panel. When multiple element phases are corrupted (right panel), the same reasoning can be applied sequentially to all the corrupted element phases to obtain the overall shift. Between all three cases, we find the SOS conservation principle to be valid. We calculate the closure phase in the image plane using the same process as employed for 3C 286 above using the principal triangle’s heights, and find it to be $112.4^\circ\pm 1.5^\circ$ on average, where the uncertainties were estimated using the uncertainties in the points of intersection determined from the peak-fitting procedure.

Figure 7.

Three element interference patterns similar to Figure 5 but for Cygnus A data. Corrupting one or all element phases results in the shifting of the interference pattern (middle and right panels) relative to the calibrated fringes (left panel), which indicates the magnitude of the required phase calibration. When a single element’s phase is corrupted by 80 $^\circ$ (middle panel), the two fringes involving that element get affected and shift while the third fringe which is unaffected. This results in the entire triangle enclosed by the fringes sliding along the uncorrupted fringe as indicated by the red double-headed arrow while preserving its shape, orientation, and size (SOS conservation). The argument can be extended to the case when all three element phases are corrupted by random amounts as representative of real-world conditions (right panel) by applying the same logic sequentially to one corrupted element phase at a time. Independent of the degree of calibration, the principal fringe NPCs in all cases are clearly non-coincident with each other which geometrically confirms that Cygnus A has a complex structure (see Figure 6) in contrast to 3C 286. Grey-shaded regions indicate twice the RMS uncertainties in the determined positions of the fringe NPCs as determined from Equation (20), but they are barely visible due to the high $S/N$ ( ${\gtrsim}275$ ) in the visibilities. The closure phase calculated from the principal triangle’s heights is ${\unicode{x03C6}}_3(\lambda)\approx 112.4^\circ$ (see Section 3.1) with an RMS uncertainty of ${\approx}1.5^\circ$ , and remains invariant even after corrupting one or more element phases by large amounts. ${\unicode{x03C6}}_3(\lambda)$ estimated from the area relations in Section 3.2 are ${\approx}112.5^\circ$ , ${\approx}113.7^\circ$ , and ${\approx}110.9^\circ$ from the fringe NPCs of the three cases considered, respectively. These images show clearly the SOS conservation principle, that is, for a closed triad of array elements, the resulting images are a true representation of the sky brightness distribution, independent of element-based phase corruption, besides an overall translation of the pattern which does not affect the SOS conservation. If the phase error was instead baseline-dependent (not shown here), only one of the NPCs that corresponds to the affected baseline will be displaced while the other two will remain unchanged and unconstrained by this phase perturbation, thereby changing the size of the resulting triangle in the image plane, as demonstrated in Figure 5 (right) for 3C 286. Thus, the SOS conservation principle will not hold for a baseline-dependent phase error.

The closure phases were also estimated using the relations between the areas in the aperture and image planes. For the chosen triad, $A_{\mathcal{A}3}(\lambda)\approx 1.976\times 10^8$ (in units of wavelengths squared). The corresponding image plane areas of the principal triangles, $A_{\mathcal{I}3}(\lambda)$ , are found to be ${\approx}1.236\times 10^{-10}$ , ${\approx}1.263\times 10^{-10}$ , and ${\approx}1.202\times 10^{-10}$ for the three cases. Hence, the respective closure phases computed are ${\approx}112.5^\circ$ , ${\approx}113.7^\circ$ , and ${\approx}110.9^\circ$ , which are consistent with the estimates above and confirm the relations derived in Section 3.

Again, although our image plane estimate appears to have a higher uncertainty, it must be noted that our aperture plane uncertainty calculation represents a best-case scenario assuming ideal thermal noise, ignoring imaging systematics around a bright, complex object such as Cygnus A. The value of closure phase inferred from the image plane is not only consistent with that estimated from the corrupted visibilities in the aperture plane, but also geometrically confirms that it is indeed independent of element-based calibration.

4.3. EHT observations of M87

As a third example, we have analysed data provided by the VLBI-based EHT observations of the supermassive black hole in M87. This example samples a very different regime in radio interferometry, namely, much higher frequencies and much longer baselines. Therefore, the data are at a much finer spatial resolution ( ${\sim}20\,\mu$ as), and the phase stability is more of a challenge relative to tied-array interferometry with the VLA.Footnote k

The EHT data (Event Horizon Telescope Collaboration 2019)Footnote l are described in detail in Event Horizon Telescope Collaboration et al. (2019c). In brief, observations were made of the nuclear regions of the nearby radio galaxy, M87 (Virgo A), with the goal of imaging the event horizon of the hypothesised supermassive black hole. Observations were made on four days at 227.1 and 229.1 GHz, each with a total bandwidth of 1.9 GHz, using an array comprised of seven telescopes spanning the globe, including Europe, South America, continental USA, and Hawaii.

The publicly available EHT data have had a priori gain (visibility flux density scale) calibration applied based on the measured system parameters at each telescope, as well as delay calibration via visibility fringe fitting, plus further adjustments based on a few redundant baselines in the array. The gain calibration provides reasonable visibility amplitudes (to within ${\sim}10\%$ ). The delay calibration provides enough phase stability to average the data in time to 10 s records, and in frequency to a single 1.875 GHz channel. Following the EHT collaboration nomenclature, we designate these data as the ‘network-calibrated data’. However, the EHT collaboration emphasises that the initial calibration alone does not allow for phase coherent imaging, since large element-based phase offsets can remain due to residual errors in the tropospheric model, station clocks, polarisation leakage, or other errors. Further element-based phase self-calibration is required to produce a phase coherent astronomical image. They state: ‘Lack of absolute phase information and a priori calibration uncertainties in EHT measurements require multiple consecutive iterations of CLEAN followed by self-calibration, a routine that solves for station gains to maximise consistency with visibilities of a specified trial image (Pearson & Readhead Reference Pearson and Readhead 1984 ).’

We have performed a standard hybrid mapping process (imaging and self-calibration; Pearson & Readhead Reference Pearson and Readhead1984), the results of which will be presented in detail in Carilli & Thyagarajan (Reference Carilli and Thyagarajan2022). Figure 8 shows the results from our hybrid mapping process of the EHT data (Carilli & Thyagarajan, Reference Carilli and Thyagarajan2022). We show the images synthesised at 229.1 GHz from the network-calibrated data, and after the hybrid mapping process in the left and right panels, respectively. The former does not produce a coherent image, due to the presence of large residual element-based phase errors. After a simple hybrid mapping and self-calibration process, the image converges to an asymmetric ring with a maximum diameter of about 50 $\mu$ as, consistent with the analysis of the EHT collaboration (Event Horizon Telescope Collaboration et al. 2019a, d).

Figure 8.

Images of M87 at 229.1 GHz made using publicly available EHT data. Left: Images from the ‘network-calibrated’ data, that is, with just a priori flux density and delay calibration that still contains residual element-based phase errors. Right: Images after hybrid mapping (iterative imaging and self-calibration) as presented in Carilli & Thyagarajan (Reference Carilli and Thyagarajan2022). The angular resolution of the image is ${\approx}20\mu$ as. The contour levels of surface brightness progress geometrically in factors of two. The contours correspond to $-3 \sigma$ (dashed), $3 \sigma$ , $6 \sigma$ , $12 \sigma$ , $24 \sigma$ , $48\sigma$ , and $96 \sigma$ , where, $\sigma\approx 0.51$ mJy beam-1 is the RMS of noise in the self-calibrated image. The colour bar uses a linear scale as indicated on the top.

Now, we present the results of the closure phase image analysis that parallels the sections above on 3C 286 and Cygnus A. For our image plane closure phase estimation, we select a short integration (1 min) with the most sensitive closed triad in the array, namely, the Atacama Large Millimeter Array (ALMA), the Large Millimeter Telescope (LMT), and the Submillimeter Array (SMA) stations. We then generate the three-fringe images under three scenarios: (i) the network-calibrated data (containing residual phase errors), (ii) the network-calibrated data, with the phase of one element further corrupted by 80 $^\circ$ , and (iii) the self-calibrated data.

The results are shown in Figure 9, from left to right, respectively. The three-fringe interference image in all scenarios are identical besides an overall shift, thus clearly demonstrating the SOS conservation principle. The three principal NPCs (black lines) determined geometrically in the image plane are also shown. The right panel shows a zoomed-in view of the triangle enclosed by the three fringe NPCs. From this triangle enclosing a finite area, we estimate the closure phase in the image plane by applying the methods described in Section 3, similar to the 3C 286 and Cygnus A examples above. The closure phase calculated from the principal triangle’s heights are 37.9 $^\circ$ , 37.4 $^\circ$ , and 41 $^\circ$ for the three scenarios, respectively, with errors ${\sim}20^\circ$ estimated from the fitting process. The closure phase estimates from the ‘product of areas’ method are 37.8 $^\circ$ , 37.1 $^\circ$ , and 40.6 $^\circ$ , respectively, for the three scenarios.

From the visibilities themselves, we derive closure phases from these three fringes to be 37.1 $^\circ$ , 37.1 $^\circ$ , and 37.9 $^\circ$ for the three scenarios, respectively. We calculate the uncertainty on these values by examining the scatter of the phases on the least sensitive baseline in the triad (LMT to SMA), over scans of 10–15 min using 1 min records. The resulting phase RMS is ${\sim}15^\circ$ . This value is consistent with the $S/N$ on that visibility, which is between 4 and 5 (Taylor et al. Reference Taylor, Carilli and Perley1999, Lecture 9 (Wrobel & Walker)). We consider this to be the RMS error on the closure phase measurements, since the RMS phase scatter on visibilities involving ALMA is more than 10 times lower, and hence does not contribute appreciably to the closure phase uncertainty.

Figure 9.

Three-fringe interference images of M87 using a snapshot (1 min) of EHT data at 229.1 GHz. The stations involved are: ALMA, the LMT, and the SMA. The first panel (from left) shows the three-fringe interference pattern that has a priori flux density scale and delay calibration applied. The second panel uses the same data but with one element (ALMA) phase-corrupted by 80 $^\circ$ . The third panel is obtained by hybrid mapping and self-calibration. The three-fringe interference pattern is found to be the same across these panels except for an overall translation relative to each other. The fourth panel is an inset showing the zoomed-in view of the self-calibrated three-fringe interference pattern. The fringe NPCs enclose a triangle of a finite area, thereby indicating a non-zero value for closure phase that was estimated from the image plane to be ${\approx}38.8^\circ$ and ${\approx}38.5^\circ$ from the ‘principal triangle’s height’ and ‘product of areas’ methods, respectively. These agree with the value of ${\approx}37.5^\circ$ derived from the aperture plane measurements (i.e., the visibilities) to within the expected uncertainties. Besides confirming that the three-fringe interference pattern remains the same except for relative overall shifts, these closure phase estimates were found to be consistent between the three panels denoting different degrees of calibration accuracy, thereby verifying the SOS conservation principle.

Once again, the image plane methods are not only consistent with each other, but also with the standard aperture plane method based on summing the visibility phases presented above. These results demonstrate that closure phases can be estimated in the image plane even in challenging interferometric experiments, such as high frequency EHT VLBI imaging of M87. Moreover, after a priori flux density calibration, Figure 9 shows that the snapshot three-fringe images are good observable representations of the true sky brightness, independent of element-based self-calibration or phase corruption, besides the overall translations. This can be compared to the network-calibrated vs self-calibrated images in Figure 9, in which the former does not produce a coherent image. The reason is, while the snapshot three-fringe images on closed baselines may be true representations of the sky, they have independent unconstrained translations that, when summed, would not produce a coherent image.